ift - User contributions [en]

Strålevern

2021-06-21T12:36:10Z

Gge002:

==Førstegangsbrukere / First-time users==
===Norsk===
Førstegangsbrukere skal:
#Ta kontakt med strålevernkoordinator (STK)
#Få de nødvendige instruksene fra STK om interne regler for bruk av strålekilder
#Bli registrert for å få personlig dosimeter
#Vente på dosimeteret (tar ca. 1-2 uker)
#Begynne å bruke kilder etter de har fått sitt personlige dosimeter
#Returnere dosimeteret sitt hvis det ikke trengs lenger (gravide brukere skal ikke jobbe med strålingskilder i løpet av svangerskapet)

===English===
First-time users shall:
#Contact the Radiation protection responsible (RPR)
#Receive the required instructions from the RPR on internal regulations for use of radioactive sources
#Be registered for obtaining a personal dosimeter
#Wait for the dosimeter (takes 1-2 weeks)
#Begin working with sources after having received her/his personal dosimeter
#Return her/his personal dosimeter if it is no longer needed (pregnant women shall not work with ionizing radiation during the pregnancy)

==Regler for bruk av strålekilder på IFT / Regulations for use of radioactive sources at the IFT==
===Norsk===
[[File:hierarket.jpg|thumb|alt=Hierarke / Hierarchy |Fig. 1 Hierarke / Hierarchy ]]
[[File:TableHeader.jpg|thumb|alt=Logbokformat / Logbook format|Fig. 2 Logbokformat / Logbook format]]
[[File:Slide2.JPG|thumb|alt=Logbokformat|Fig. 3 Skilt som brukes til svake kilder / Sign used for designating an area where weak sources are used]]
[[File:Slide1.JPG|thumb|alt=Logbokformat|Fig. 4 Skilt som brukes til sterke kilder og kontaminerte områder hvor begrenset opphold er bare tillatt / Sign used for designating an area where strong sources are used, or for contaminated areas, where only a limited time presence is allowed]]

#Strålevernkoordinatoren (STK) har oversikt over alle kildenes status.
#Ansvarshierarkiet er som vist i Fig. 1.
#Hver lab bør ha lab kildeansvarlig. I tilfelle det ikke er lab-kildeansvarlig deles kildene ut av STK.
#Lab-kildeansvarlig velges av lab-brukerne, STK eller instituttleder.
#Hver lab skal ha loggbok hvor bevegelsene til hver kilde som hører til denne laben skal registreres. Loggboken skal ha formatet som vist i Fig. 2:
#Den første siden i loggboken skal ha navn og kontaktinfo til lab kildeansvarlig og navn og kontakt info til STK.
#Loggboken skal være på labben til enhver tid, bundet med snor til kildeskapet.
#Det er lab kildeansvarlig sitt ansvar å føre boken riktig.
#STK skal kontrollere jobben til lab-kildeansvarlig ofte og uten varsel.
#Det er 1 nøkkel til tilsvarende kildeskap hos lab-kildeansvarlig og 1 nøkkel hos STK. Leder for teknisk Avdeling (TA) og 1 ingeniør fra TA skal kunne få tilgang til STK sine nøkler i tilfelle STK ikke er tilstede.
#Alle personer som har tilgang til nøkler til kildeskap får opplæring i dette regelverket og generell strålevern fra STK.
#Ingen av ovennevnte får lov til å låne sin nøkkel til noen. STK kan delegere ansvaret for nøklene sine, men overføringen skal skje med overtagelsesprotokoll som er en del av loggboken. Lab-kildeansvarlig kan IKKE delegere sitt ansvar for nøkkelen.
#En kildebruker skal først ta kontakt med sin lab-kildeansvarlig. Hvis han/hun ikke er tilstede kontaktes STK. Hvis han/hun ikke er til stedet kontaktes leder TA. Hvis han/hun ikke er til stedet kontaktes ingeniøren som er ansvarlig. Det er IKKE lov å hoppe over noen.
#Hvis lab kildeansvarlig sier opp blir det varetelling med STK og instituttleder og signering av overtagelsesprotokoll.
#Hvis STK sier opp blir det varetelling med UiB STK, instituttleder og den nye STK. Overtagelsesprotokoll signeres.
#Arbeidsplass med åpen strålekilde skal merkeres med skilt (Fig. 3 eller Fig. 4) og eksponeringsvurdering skal utføres om nødvendig.
#Det er ikke ønskelig å la kilder stå uovervåket. Hvis dette er nødvendig skal arbeidstedet markeres.
#Det er ikke lov å jobbe med strålekilder uten dosimeter. STK og HMS-ansvarlig skal kontrollere labbene og brukerne uten varsel.
#Hver bruker skal ha innføring i strålevern fra STK før de begynner å jobbe med kilder. Studenter som har bestått PHYS231 Strålingsfysikk får fritak.
#Gravide brukere skal returnere sine dosimetere til HMS-ansvarlige i det øyeblikket de finner ut at de er gravide (se punkt 18). Dosimeteret blir returnert etter fødsel om det fremdeles er ønskelig.
#Brukere som ikke har bruk for dosimeter lenger skal returnere dem til HMS ansvarlig.
#Dosimetrene skal oppbevares på samme sted når de ikke er i bruk. Det stede skal bestemmes mellom bruker, STK og personen som er ansvarlig for den periodiske skift av TLD.
#De personlige dosimetrene skal brukes bare på IFT og skal ikke taes fra huset. Dette inkluderer ansatte som jobber på eksterne fasiliteter som f.eks. CERN. Sånne ansatte får dosimetrer fra fasilitetene de besøker.

===English===
#The Radiation protection responsible (RPR) has all the information on the status of the radioactive sources at the IFT.
#The hierarchy and the responsibilities are defined in Fig. 1.
#Every lab should have a responsible for the radioactive sources. During the absence of the lab responsible it is the RPR who gives out sources.
#The lab responsible is elected by the users in that lab, RPR or the Head of the department.
#Every lab will have a logbook where the movement of all the sources belonging to this lab will be registered. The format of the logbook will be as shown in Fig. 2.
#The first page in the logbook will contain the name and the contact info of the lab responsible and the name and the contact info of the RPR.
#The logbook will be in the lab at all times, bound to the safe with the sources with the help of a thread.
#It is the responsibility of the lab responsible to keep the book correctly.
#RPR shall inspect the work of the lab responsible often and without warning.
#There is one key per safe in the possession of the lab responsible and one key with the RPR. Head of Technical department and one engineer shall be able to access to the keys belonging to the RPR in case the RPR is absent.
#All persons who have access to keys for the safes with radioactive sources shall be briefed on this framework of rules and on general radiation protection by the RPR.
#Nobody from the aforementioned personnel is allowed to lend their keys to anyone. RPR can delegate the responsibility for a certain safe, but this will happen with a protocol. The protocol is a part of the logbook. The lab responsible is not allowed to delegate her/his responsibilities.
#The users will first contact their lab responsible. If she/he are not present, the RPR is to be contacted. If she/he is not present the Head of the Technical department is to be contacted. If she/he is not present the authorized engineer is to be contacted.
#When the lab responsible quits there will be an inspection of the inventory with the RPR and the Head of the Department, followed by signing a transfer protocol.
#When the RPR quits there will be an inventory inspection together with the UiB RPR, the Head of the Department and the new RPR. This will result in signing a transfer protocol.
#Workplace with an open radioactive source will be marked with a shield (Fig. 3 or Fig. 4) and there shall be a dose estimate if needed.
#It is undesirable to leave sources unattended. If this is necessary, the work place shall be marked accordingly.
#It is forbidden to work with radioactive sources without a dosimeter. The RPR and HSE responsible will the labs and the users without warning.
#Every new user shall receive an introduction in radiation protection by the RPR before beginning to work with radioactive sources. Students who have successfully passed PHYS231 Strålingsfysikk or equivalent are exempt.
#Pregnant users shall return their dosimeters to the HSE responsible in the moment they discover they are pregnant (see item 18). The dosimeters shall be returned after birth if they are still needed.
#Users who no longer need their dosimeters shall return them to the HSE responsible.
#The dosimeters shall be stored in the same place whenever they are no in use. That place is agreed upon between the user, the RPR and the person responsible for the periodic change of the TLD.
#The personal dosimeter shall be used only when working at the IFT and shall be located at the IFT building at all times. This includes students and employees who work at external organizations like CERN. Such employees and students receive dosimeters at the institutions they visit.

==List of sealed sources at the IFT==

===Storage 4===
{| class="wikitable"
|-
! Item
! Source ID
! Isotope
! Activity, µCi
! Aktivity, kBq
! Year
! Half-life
! Radiation type
! Note
|-
| 1
| Storage 4 #1
| 241Am
| 27
| 1 000
| 2006
| 458 y
| 60 keV gamma
| OI428/Code: AMRB 13788
|-
| 2
| Storage 4 #2
| 57Co
| 100
| 3 700
| 2006
| 272 d
| 122 keV gamma
| Code: CTR 8252
|-
| 3
| Storage 4 #3
| 133Ba
| 100
| 3 700
| 2006
| 10.5 y
| 80, 276, 303, 356, 384 keV gamma
| Code: BDR 8252
|-
| 4
| Storage 4 #4
| 155Eu
| 100
| 3 700
| 1993
| 4.8 y
| 105 keV gamma
|
|-
| 5
| Storage 4 #5
| 226Ra
| 2.7
| 100
| ~1970
| 1 600 y
| 186 keV gamma
|
|-
| 6
| Storage 4 #6
| 137Cs
| 60
| 2 200
| 1986
| 30 y
| 662 keV gamma
|
|-
| 7
| Storage 4 #7
| 241Am
| 3 000
| 100 000
| 1977
| 458 y
| 60 keV gamma
| UB/FIB 539
|-
| 8
| Storage 4 #8
| 241Am
| 10 000
| 370 000
| 1987
| 458 y
|
| Variable X-ray source
|-
| 9
| Storage 4 #9
| 55Fe
| 20 000
| 740 000
| N/A
| 2.7 y
| X-rays
| Decayed
|-
| 10
| Storage 4 #10
| 109Cd
| 1
| 37
| 2011
| 427 d
| 88 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 11
| Storage 4 #11
| 57Co
| 1
| 37
| 2011
| 272 d
| 122 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 12
| Storage 4 #12
| 133Ba
| 1
| 37
| 2011
| 10.5 y
| 80, 276, 303, 356, 384 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 13
| Storage 4 #13
| 60Co
| 1
| 37
| 2011
| 5.3 y
| 1 173, 1 333 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 14
| Storage 4 #14
| 137Cs
| 1
| 37
| 2011
| 30 y
| 662 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 15
| Storage 4 #15
| 22Na
| 1
| 37
| 2011
| 2.6 y
| 511, 1 275 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 16
| Storage 4 #16
| 137Cs65Zn
| 1
| 37
| 2011
| 30 y + 244 d
| 662 + 1 116 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 17
| Storage 4 #17
| 54Mn
| 1
| 37
| 2011
| 312 d
| 835 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 18
| Storage 4 #18
| 137Cs
| 10
| 370
| 2011
| 30 y
| 662 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 19
| Storage 4 #19
| 22Na
| 10
| 370
| 2011
| 2.6 y
| 511, 1 275 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 20
| Storage 4 #20
| 54Mn
| 10
| 370
| 2011
| 312 d
| 835 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 21
| Storage 4 #21
| 133Ba
| 10
| 370
| 2012
| 10.5 y
| 80, 276, 303, 356, 384 keV gamma
| Calibr. source Eckert & Ziegler
|-
| 22
| Storage 4 #22
| 241Am
| 1
| 37
| 1990
| 458 y
| 60 keV gamma
| Laborel box (ruined and sagregated for disposal)
|-
| 23
| Storage 4 #23
| 109Cd
| 1
| 37
| 1990
| 427 d
| 88 keV gamma
| Laborel box
|-
| 24
| Storage 4 #24
| 139Ce
| 1
| 37
| 1990
| 138 d
| 166 keV gamma
| Laborel box
|-
| 25
| Storage 4 #25
| 57Co
| 1
| 37
| 1990
| 272 d
| 122 keV gamma
| Laborel box
|-
| 26
| Storage 4 #26
| 137Cs
| 1
| 37
| 1190
| 30 y
| 662 keV gamma
| Laborel box
|-
| 27
| Storage 4 #27
| 51Cr
| 1
| 37
| 1990
| 27 d
| 320 keV gamma
| Laborel box
|-
| 28
| Storage 4 #28
| 54Mn
| 1
| 37
| 1990
| 312 d
| 835 keV gamma
| Laborel box
|-
| 29
| Storage 4 #29
| 113Sn
| 1
| 37
| 1990
| 115 d
| 255 keV gamma
| Laborel box
|-
| 30
| Storage 4 #30
| 85Sr
| 1
| 37
| 1990
| 65 d
| 355 keV gamma
| Laborel box
|-
| 31
| Storage 4 #31
| 65Zn
| 1
| 37
| 1990
| 244 d
| 1 116 keV gamma
| Laborel box
|-
| 32
| Storage 4 #32
| 133Ba
| 4 000
| 148 000
| 2014
| 10.5 y
| 80, 276, 303, 356, 384 keV gamma
| Eckert & Ziegler, Brass holder
|-
| 33
| Storage 4 #33
| 90Sr
| 54
| 2 010
| 1993
| 29 y
| e-
| DESY
|-
| 34
| Storage 4 #34
| 55Fe
| 1 000
| 37 000
| 2014
| 2.7 y
| X-rays
| UiB# 0218698
|-
| 35
| Storage 4 #35a
| 14C
| 10
| 370
| 2018
| 5730 y
| e-
| Thin plate; Spec. Tech. Mod# C14LMW10
|-
| 36
| Storage 4 #35b
| 14C
| 10
| 370
| 2018
| 5730 y
| e-
| Thin plate; Spec. Tech. Mod# C14LMW10
|-
|}

===Storage 3===
{| class="wikitable"
|-
! Item
! Source ID
! Isotope
! Activity, µCi
! Aktivity, kBq
! Year
! Half-life
! Radiation type
! Note
|-
| 1
| Storage 3 #1
| 60Co
| 5
| 185
| 1972
| 5.3 y
| 1 173, 1 333 keV gamma
|
|-
| 2
| Storage 3 #2
| 133Ba
| 1
| 37
| 2013
| 10.5 y
| 80, 276, 303, 356, 384 keV gamma
|
|-
| 3
| Storage 3 #3
| 22Na
| 1
| 37
| 2013
| 2.6 y
| 511, 1 275 keV gamma
|
|-
| 4
| Storage 3 #4
| 57Co
| 1
| 37
| 2013
| 272 d
| 122 keV gamma
|
|-
| 5
| Storage 3 #5a
| 60Co
| 1
| 37
| 2005
| 5.3 y
| 1 173, 1 333 keV gamma
|
|-
| 6
| Storage 3 #5b
| 60Co
| 1
| 37
| 2005
| 5.3 y
| 1 173, 1 333 keV gamma
|
|-
| 7
| Storage 3 #6
| 137Cs
| 5
| 185
| 1999
| 30 y
| 662 keV gamma
|
|-
| 8
| Storage 3 #7
| 241Am
| 1
| 37
| 1976
| 458 y
| Alpha + 60 keV gamma
| Glass tube set
|-
| 9
| Storage 3 #8
| 90Sr
| 1
| 37
| 1976
| 29 y
| e-
| Glass tube set
|-
| 10
| Storage 3 #9
| 55Fe
| 10
| 370
| 1976
| 30 y
| 662 keV gamma
| Glass tube set
|-
| 11
| Storage 3 #10
| 106Ru
| 2.7
| 100
| 2000
| 374 d
| e-
|
|-
| 12
| Storage 3 #11
| 241Am
| 10
| 370
| 1975
| 458 y
| Alpha + 60 keV gamma
| ORTEC AM-1U, S/N M-1343, act. 0.088
|-
|}

===Storage 2===
{| class="wikitable"
|-
! Item
! Source ID
! Isotope
! Activity, µCi
! Aktivity, kBq
! Year
! Half-life
! Radiation type
! Note
|-
| 1
| Storage 2 #1a
| 137Cs
| 5
| 185
| 2003
| 30 y
| 662 keV gamma
|
|-
| 2
| Storage 2 #1b
| 137Cs
| 5
| 185
| 2003
| 30 y
| 662 keV gamma
|
|-
| 3
| Storage 2 #1c
| 137Cs
| 5
| 185
| 2003
| 30 y
| 662 keV gamma
|
|-
| 4
| Storage 2 #1d
| 137Cs
| 5
| 185
| 2003
| 30 y
| 662 keV gamma
|
|-
| 5
| Storage 2 #1e
| 137Cs
| 5
| 185
| 2003
| 30 y
| 662 keV gamma
|
|-
| 6
| Storage 2 #1f
| 137Cs
| 5
| 185
| 2003
| 30 y
| 662 keV gamma
|
|-
| 7
| Storage 2 #2
| 137Cs
| 5
| 185
| 1999
| 30 y
| 662 keV gamma
|
|-
| 8
| Storage 2 #3a
| 90Sr
| 0.1
| 3.7
| 2005
| 29 y
| e-
|
|-
| 9
| Storage 2 #3b
| 90Sr
| 0.1
| 3.7
| 2005
| 29 y
| e-
|
|-
| 10
| Storage 2 #4a
| 210Po
| 0.1
| 3.7
| 2005
| 138 d
| 803 keV gamma
|
|-
| 11
| Storage 2 #4b
| 210Po
| 0.1
| 3.7
| 2005
| 138 d
| 803 keV gamma
|
|-
| 12
| Storage 2 #5a
| 137Cs
| 5
| 185
| 1972
| 30 y
| 662 keV gamma
|
|-
| 13
| Storage 2 #5b
| 137Cs
| 5
| 185
| 1972
| 30 y
| 662 keV gamma
|
|-
| 14
| Storage 2 #6
| 60Co
| 5
| 185
| 1972
| 5.3 y
| 1 173, 1 333 keV gamma
|
|-
| 15
| Storage 2 #7
| 152Eu
| 0.04
| 1.5
| 2006
| 13.5 y
| Many gamma lines
| Sealed Liquid
|-
| 16
| Storage 2 #8a
| 22Na
| 1
| 37
| 2005
| 2.6 y
| 511, 1 275 keV gamma
|
|-
| 17
| Storage 2 #8b
| 22Na
| 1
| 37
| 2005
| 2.6 y
| 511, 1 275 keV gamma
|
|-
| 18
| Storage 2 #8c
| 22Na
| 1
| 37
| 2005
| 2.6 y
| 511, 1 275 keV gamma
|
|-
| 19
| Storage 2 #9a
| 137Cs
| 0.5
| 18.5
| 2005
| 30 y
| 662 keV gamma
|
|-
| 20
| Storage 2 #9b
| 137Cs
| 0.5
| 18.5
| 2005
| 30 y
| 662 keV gamma
|
|-
| 21
| Storage 2 #9c
| 137Cs
| 0.5
| 18.5
| 2005
| 30 y
| 662 keV gamma
|
|-
| 22
| Storage 2 #9d
| 137Cs
| 0.5
| 18.5
| 2005
| 30 y
| 662 keV gamma
|
|-
| 23
| Storage 2 #10
| 152Eu
| 1
| 37
| 2005
| 13.5 y
| Many gamma lines
|
|-
| 24
| Storage 2 #11a
| 204Tl
| 10
| 370
| 1993
| 3.78 y
| 511 keV gamma
| Al housing
|-
| 25
| Storage 2 #11b
| 204Tl
| 10
| 370
| 1993
| 3.78 y
| 511 keV gamma
| Al housing
|-
| 26
| Storage 2 #11c
| 204Tl
| 10
| 370
| 1993
| 3.78 y
| 511 keV gamma
| Al housing
|-
| 27
| Storage 2 #11d
| 204Tl
| 10
| 370
| 1993
| 3.78 y
| 511 keV gamma
| Al housing
|-
| 28
| Storage 2 #12a
| 226Ra
| 0.09
| 3.3
| 2005
| 1 600 y
| 186 keV gamma
| Glass jar
|-
| 29
| Storage 2 #12b
| 226Ra
| 0.09
| 3.3
| 2005
| 1 600 y
| 186 keV gamma
| Glass jar
|-
| 30
| Storage 2 #12c
| 226Ra
| 0.09
| 3.3
| 2005
| 1 600 y
| 186 keV gamma
| Glass jar
|-
| 31
| Storage 2 #13
| 241Am
| 0.24
| 9
| N/A
| 458 y
| 60 keV gamma
| GDM 625
|-
| 32
| Storage 2 #14
| 137Cs
| 1.22
| 45
| N/A
| 30 y
| 662 keV gamma
| GDM 134
|-
| 33
| Storage 2 #15
| UO2
| N/A
| N/A
| N/A
| N/A
| N/A
| Nuclear fuel pellet (black cylinder in epoxy cube)
|-
|}

===Storage 1===
====White====
{| class="wikitable"
|-
! Item
! Source ID
! Isotope
! Activity, µCi
! Aktivity, kBq
! Year
! Half-life
! Radiation type
! Note
|-
| 1
| Storage 1W #1
| 241Am
| 10 000
| 370 000
|
| 458 y
| X-rays
| Variable X-ray source
|-
| 2
| Storage 1W #2
| 241Am
| 10
| 370
| 1993
| 458 y
| 60 keV gamma
| DA289 written on the source
|-
| 3
| Storage 1W #3
| 60Co
| 10
| 370
| 1970
| 10.5 y
| 1 173, 1 333 keV gamma
| A943F
|-
| 4
| Storage 1W #4
| 147Pm
| 10 000
| 370 000
| 1974
| 2.6 y
| 76, 198 keV gamma
| A1124/N11958
|-
| 5
| Storage 1W #5
| 137Cs
| 10
| 370
|
| 30 y
| 662 keV gamma
| S/N 15319; A919F
|-
| 6
| Storage 1W #6
| 60Co
| 1
| 37
|
| 10.5 y
| 1 173, 1 333 keV gamma
| S/N 811-L-1
|-
| 7
| Storage 1W #7
| 241Am
| 0.1
| 3.7
| 1966
| 458 y
| 60 keV gamma
| A922F; S/N M954 Ortec
|-
| 8
| Storage 1W #8
| 241Am
| 10 000
| 370 000
| 2010
| 458 y
| 60 keV gamma
|
|-
| 9
| Storage 1W #9
| 137Cs
| 100
| 3 700
| 1984
| 30 y
| 662 keV gamma
|
|-
| 10
| Storage 1W #10
| 241Am
| 14 000
| 518 000
| 1984
| 458 y
| 60 keV gamma
| M55005
|-
| 11
| Storage 1W #11
| 241Am
| 10 000
| 370 000
| 2010
| 458 y
| 60 keV gamma
|
|-
| 12
| Storage 1W #12
| 226Ra
| 5-10
| 185-370
| 1970
| 1 600 y
| 186 keV gamma
| A859F; Leybold in a jar
|-
| 13
| Storage 1W #13
| 137Cs
| <10
| <370
| 2005
| 30 y
| 662 keV gamma
| Isotope generator
|-
| 14
| Storage 1W #14a
| 238U
| 1
| 37
| 2006
| 4.5e9 y
| 50, 114 keV gamma + alpha
| Liquid in plastic bottles (B. Stugu’s)
|-
| 15
| Storage 1W #14b
| 238U
| 1
| 37
| 2006
| 4.5e9 y
| 50, 114 keV gamma + alpha
| Liquid in plastic bottles (B. Stugu’s)
|-
| 16
| Storage 1W #14c
| 238U
| 1
| 37
| 2006
| 4.5e9 y
| 50, 114 keV gamma + alpha
| Liquid in plastic bottles (B. Stugu’s)
|-
| 17
| Storage 1W #15
| 90Sr
| 2 000
| 74 000
| 1987
| 29 y
| e-
| Amersham (in a blue cylindrical collimator)
|-
| 18
| Storage 1W #16
|
|
|
| 1945
|
|
| Hiroshima dust
|-
| 19
|
|
| 0
| 0
| 2005
|
|
| Eluting solution for Tilf #13 Isotope generator
|-
|}
====Black====
{| class="wikitable"
|-
! Item
! Source ID
! Activity, counts/s*
! Note
|-
| 1
| Storage 1B #1
| ~20
| Storage 1B R. 1
|-
| 2
| Storage 1B #2
| ~120
| Storage 1B G. 1
|-
| 3
| Storage 1B #3
| ~60
| Storage 1B G. 2
|-
| 4
| Storage 1B #4
| ~100
| Storage 1B G. 3
|-
| 5
| Storage 1B #5
| ~10
| Storage 1B G. 4
|-
| 6
| Storage 1B #6
| ~10
| Storage 1B G. 5
|-
| 7
| Storage 1B #7
| ~0
| Storage 1B G. 6
|-
| 8
| Storage 1B #8
| ~220
| Storage 1B G. 7
|-
| 9
| Storage 1B #9
| ~150
| Storage 1B G. 8
|-
| 10
| Storage 1B #10
| ~10
| Storage 1B G. 9
|-
| 11
| Storage 1B #11
| ~350
| Storage 1B G. 10
|-
| 12
| Storage 1B #12
| ~500
| Storage 1B G. 11
|-
| 13
| Storage 1B #13
| ~1 000
| Storage 1B G. 12
|-
|}
<nowiki>*</nowiki>Activity measured with an 1" NaI(Tl) crystal

Strålevern

2018-11-16T17:45:58Z

Gge002:

==Førstegangsbrukere / First-time users==
===Norsk===
Førstegangsbrukere skal:
#Ta kontakt med strålevernkoordinator (STK)
#Få de nødvendige instruksene fra STK om interne regler for bruk av strålekilder
#Bli registrert for å få personlig dosimeter
#Vente på dosimeteret (tar ca. 1-2 uker)
#Begynne å bruke kilder etter de har fått sitt personlige dosimeter
#Returnere dosimeteret sitt hvis det ikke trengs lenger (gravide brukere skal ikke jobbe med strålingskilder i løpet av svangerskapet)

===English===
First-time users shall:
#Contact the Radiation protection responsible (RPR)
#Receive the required instructions from the RPR on internal regulations for use of radioactive sources
#Be registered for obtaining a personal dosimeter
#Wait for the dosimeter (takes 1-2 weeks)
#Begin working with sources after having received her/his personal dosimeter
#Return her/his personal dosimeter if it is no longer needed (pregnant women shall not work with ionizing radiation during the pregnancy)

==Regler for bruk av strålekilder på IFT / Regulations for use of radioactive sources at the IFT==
===Norsk===
[[File:hierarket.jpg|thumb|alt=Hierarke / Hierarchy |Fig. 1 Hierarke / Hierarchy ]]
[[File:TableHeader.jpg|thumb|alt=Logbokformat / Logbook format|Fig. 2 Logbokformat / Logbook format]]
[[File:Slide2.JPG|thumb|alt=Logbokformat|Fig. 3 Skilt som brukes til svake kilder / Sign used for designating an area where weak sources are used]]
[[File:Slide1.JPG|thumb|alt=Logbokformat|Fig. 4 Skilt som brukes til sterke kilder og kontaminerte områder hvor begrenset opphold er bare tillatt / Sign used for designating an area where strong sources are used, or for contaminated areas, where only a limited time presence is allowed]]

#Strålevernkoordinatoren (STK) har oversikt over alle kildenes status.
#Ansvarshierarkiet er som vist i Fig. 1.
#Hver lab bør ha lab kildeansvarlig. I tilfelle det ikke er lab-kildeansvarlig deles kildene ut av STK.
#Lab-kildeansvarlig velges av lab-brukerne, STK eller instituttleder.
#Hver lab skal ha loggbok hvor bevegelsene til hver kilde som hører til denne laben skal registreres. Loggboken skal ha formatet som vist i Fig. 2:
#Den første siden i loggboken skal ha navn og kontaktinfo til lab kildeansvarlig og navn og kontakt info til STK.
#Loggboken skal være på labben til enhver tid, bundet med snor til kildeskapet.
#Det er lab kildeansvarlig sitt ansvar å føre boken riktig.
#STK skal kontrollere jobben til lab-kildeansvarlig ofte og uten varsel.
#Det er 1 nøkkel til tilsvarende kildeskap hos lab-kildeansvarlig og 1 nøkkel hos STK. Leder for teknisk Avdeling (TA) og 1 ingeniør fra TA skal kunne få tilgang til STK sine nøkler i tilfelle STK ikke er tilstede.
#Alle personer som har tilgang til nøkler til kildeskap får opplæring i dette regelverket og generell strålevern fra STK.
#Ingen av ovennevnte får lov til å låne sin nøkkel til noen. STK kan delegere ansvaret for nøklene sine, men overføringen skal skje med overtagelsesprotokoll som er en del av loggboken. Lab-kildeansvarlig kan IKKE delegere sitt ansvar for nøkkelen.
#En kildebruker skal først ta kontakt med sin lab-kildeansvarlig. Hvis han/hun ikke er tilstede kontaktes STK. Hvis han/hun ikke er til stedet kontaktes leder TA. Hvis han/hun ikke er til stedet kontaktes ingeniøren som er ansvarlig. Det er IKKE lov å hoppe over noen.
#Hvis lab kildeansvarlig sier opp blir det varetelling med STK og instituttleder og signering av overtagelsesprotokoll.
#Hvis STK sier opp blir det varetelling med UiB STK, instituttleder og den nye STK. Overtagelsesprotokoll signeres.
#Arbeidsplass med åpen strålekilde skal merkeres med skilt (Fig. 3 eller Fig. 4) og eksponeringsvurdering skal utføres om nødvendig.
#Det er ikke ønskelig å la kilder stå uovervåket. Hvis dette er nødvendig skal arbeidstedet markeres.
#Det er ikke lov å jobbe med strålekilder uten dosimeter. STK og HMS-ansvarlig skal kontrollere labbene og brukerne uten varsel.
#Hver bruker skal ha innføring i strålevern fra STK før de begynner å jobbe med kilder. Studenter som har bestått PHYS231 Strålingsfysikk får fritak.
#Gravide brukere skal returnere sine dosimetere til HMS-ansvarlige i det øyeblikket de finner ut at de er gravide (se punkt 18). Dosimeteret blir returnert etter fødsel om det fremdeles er ønskelig.
#Brukere som ikke har bruk for dosimeter lenger skal returnere dem til HMS ansvarlig.
#Dosimetrene skal oppbevares på samme sted når de ikke er i bruk. Det stede skal bestemmes mellom bruker, STK og personen som er ansvarlig for den periodiske skift av TLD.
#De personlige dosimetrene skal brukes bare på IFT og skal ikke taes fra huset. Dette inkluderer ansatte som jobber på eksterne fasiliteter som f.eks. CERN. Sånne ansatte får dosimetrer fra fasilitetene de besøker.

===English===
#The Radiation protection responsible (RPR) has all the information on the status of the radioactive sources at the IFT.
#The hierarchy and the responsibilities are defined in Fig. 1.
#Every lab should have a responsible for the radioactive sources. During the absence of the lab responsible it is the RPR who gives out sources.
#The lab responsible is elected by the users in that lab, RPR or the Head of the department.
#Every lab will have a logbook where the movement of all the sources belonging to this lab will be registered. The format of the logbook will be as shown in Fig. 2.
#The first page in the logbook will contain the name and the contact info of the lab responsible and the name and the contact info of the RPR.
#The logbook will be in the lab at all times, bound to the safe with the sources with the help of a thread.
#It is the responsibility of the lab responsible to keep the book correctly.
#RPR shall inspect the work of the lab responsible often and without warning.
#There is one key per safe in the possession of the lab responsible and one key with the RPR. Head of Technical department and one engineer shall be able to access to the keys belonging to the RPR in case the RPR is absent.
#All persons who have access to keys for the safes with radioactive sources shall be briefed on this framework of rules and on general radiation protection by the RPR.
#Nobody from the aforementioned personnel is allowed to lend their keys to anyone. RPR can delegate the responsibility for a certain safe, but this will happen with a protocol. The protocol is a part of the logbook. The lab responsible is not allowed to delegate her/his responsibilities.
#The users will first contact their lab responsible. If she/he are not present, the RPR is to be contacted. If she/he is not present the Head of the Technical department is to be contacted. If she/he is not present the authorized engineer is to be contacted.
#When the lab responsible quits there will be an inspection of the inventory with the RPR and the Head of the Department, followed by signing a transfer protocol.
#When the RPR quits there will be an inventory inspection together with the UiB RPR, the Head of the Department and the new RPR. This will result in signing a transfer protocol.
#Workplace with an open radioactive source will be marked with a shield (Fig. 3 or Fig. 4) and there shall be a dose estimate if needed.
#It is undesirable to leave sources unattended. If this is necessary, the work place shall be marked accordingly.
#It is forbidden to work with radioactive sources without a dosimeter. The RPR and HSE responsible will the labs and the users without warning.
#Every new user shall receive an introduction in radiation protection by the RPR before beginning to work with radioactive sources. Students who have successfully passed PHYS231 Strålingsfysikk or equivalent are exempt.
#Pregnant users shall return their dosimeters to the HSE responsible in the moment they discover they are pregnant (see item 18). The dosimeters shall be returned after birth if they are still needed.
#Users who no longer need their dosimeters shall return them to the HSE responsible.
#The dosimeters shall be stored in the same place whenever they are no in use. That place is agreed upon between the user, the RPR and the person responsible for the periodic change of the TLD.
#The personal dosimeter shall be used only when working at the IFT and shall be located at the IFT building at all times. This includes students and employees who work at external organizations like CERN. Such employees and students receive dosimeters at the institutions they visit.

==List of sealed sources at the IFT==

===Storage 4===
{| class="wikitable"
|-
! Item
! Source ID
! Isotope
! Activity, µCi
! Aktivity, kBq
! Year
! Half-life
! Radiation type
! Note
|-
| 1
| Storage 4 #1
| 241Am
| 27
| 1 000
| 2006
| 458 y
| 60 keV gamma
| OI428/Code: AMRB 13788
|-
| 2
| Storage 4 #2
| 57Co
| 100
| 3 700
| 2006
| 272 d
| 122 keV gamma
| Code: CTR 8252
|-
| 3
| Storage 4 #3
| 133Ba
| 100
| 3 700
| 2006
| 10.5 y
| 80, 276, 303, 356, 384 keV gamma
| Code: BDR 8252
|-
| 4
| Storage 4 #4
| 155Eu
| 100
| 3 700
| 1993
| 4.8 y
| 105 keV gamma
|
|-
| 5
| Storage 4 #5
| 226Ra
| 2.7
| 100
| ~1970
| 1 600 y
| 186 keV gamma
|
|-
| 6
| Storage 4 #6
| 137Cs
| 60
| 2 200
| 1986
| 30 y
| 662 keV gamma
|
|-
| 7
| Storage 4 #7
| 241Am
| 3 000
| 100 000
| 1977
| 458 y
| 60 keV gamma
| UB/FIB 539
|-
| 8
| Storage 4 #8
| 241Am
| 10 000
| 370 000
| 1987
| 458 y
|
| Variable X-ray source
|-
| 9
| Storage 4 #9
| 55Fe
| 20 000
| 740 000
| N/A
| 2.7 y
| X-rays
| Decayed
|-
| 10
| Storage 4 #10
| 109Cd
| 1
| 37
| 2011
| 427 d
| 88 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 11
| Storage 4 #11
| 57Co
| 1
| 37
| 2011
| 272 d
| 122 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 12
| Storage 4 #12
| 133Ba
| 1
| 37
| 2011
| 10.5 y
| 80, 276, 303, 356, 384 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 13
| Storage 4 #13
| 60Co
| 1
| 37
| 2011
| 5.3 y
| 1 173, 1 333 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 14
| Storage 4 #14
| 137Cs
| 1
| 37
| 2011
| 30 y
| 662 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 15
| Storage 4 #15
| 22Na
| 1
| 37
| 2011
| 2.6 y
| 511, 1 275 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 16
| Storage 4 #16
| 137Cs65Zn
| 1
| 37
| 2011
| 30 y + 244 d
| 662 + 1 116 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 17
| Storage 4 #17
| 54Mn
| 1
| 37
| 2011
| 312 d
| 835 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 18
| Storage 4 #18
| 137Cs
| 10
| 370
| 2011
| 30 y
| 662 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 19
| Storage 4 #19
| 22Na
| 10
| 370
| 2011
| 2.6 y
| 511, 1 275 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 20
| Storage 4 #20
| 54Mn
| 10
| 370
| 2011
| 312 d
| 835 keV gamma
| Calibr. Set Spectrum Techniques
|-
| 21
| Storage 4 #21
| 133Ba
| 10
| 370
| 2012
| 10.5 y
| 80, 276, 303, 356, 384 keV gamma
| Calibr. source Eckert & Ziegler
|-
| 22
| Storage 4 #22
| 241Am
| 1
| 37
| 1990
| 458 y
| 60 keV gamma
| Laborel box (ruined and sagregated for disposal)
|-
| 23
| Storage 4 #23
| 109Cd
| 1
| 37
| 1990
| 427 d
| 88 keV gamma
| Laborel box
|-
| 24
| Storage 4 #24
| 139Ce
| 1
| 37
| 1990
| 138 d
| 166 keV gamma
| Laborel box
|-
| 25
| Storage 4 #25
| 57Co
| 1
| 37
| 1990
| 272 d
| 122 keV gamma
| Laborel box
|-
| 26
| Storage 4 #26
| 137Cs
| 1
| 37
| 1190
| 30 y
| 662 keV gamma
| Laborel box
|-
| 27
| Storage 4 #27
| 51Cr
| 1
| 37
| 1990
| 27 d
| 320 keV gamma
| Laborel box
|-
| 28
| Storage 4 #28
| 54Mn
| 1
| 37
| 1990
| 312 d
| 835 keV gamma
| Laborel box
|-
| 29
| Storage 4 #29
| 113Sn
| 1
| 37
| 1990
| 115 d
| 255 keV gamma
| Laborel box
|-
| 30
| Storage 4 #30
| 85Sr
| 1
| 37
| 1990
| 65 d
| 355 keV gamma
| Laborel box
|-
| 31
| Storage 4 #31
| 65Zn
| 1
| 37
| 1990
| 244 d
| 1 116 keV gamma
| Laborel box
|-
| 32
| Storage 4 #32
| 133Ba
| 4 000
| 148 000
| 2014
| 10.5 y
| 80, 276, 303, 356, 384 keV gamma
| Eckert & Ziegler, Brass holder
|-
| 33
| Storage 4 #33
| 90Sr
| 54
| 2 010
| 1993
| 29 y
| e-
| DESY
|-
| 34
| Storage 4 #34
| 55Fe
| 1 000
| 37 000
| 2014
| 2.7 y
| X-rays
| UiB# 0218698
|-
| 35
| Storage 4 #35a
| 14C
| 10
| 370
| 2018
| 5730 y
| e-
| Thin plate; Spec. Tech. Mod# C14LMW10
|-
| 36
| Storage 4 #35b
| 14C
| 10
| 370
| 2018
| 5730 y
| e-
| Thin plate; Spec. Tech. Mod# C14LMW10
|-
|}

===Storage 3===
{| class="wikitable"
|-
! Item
! Source ID
! Isotope
! Activity, µCi
! Aktivity, kBq
! Year
! Half-life
! Radiation type
! Note
|-
| 1
| Storage 3 #1
| 60Co
| 5
| 185
| 1972
| 5.3 y
| 1 173, 1 333 keV gamma
|
|-
| 2
| Storage 3 #2
| 133Ba
| 1
| 37
| 2013
| 10.5 y
| 80, 276, 303, 356, 384 keV gamma
|
|-
| 3
| Storage 3 #3
| 22Na
| 1
| 37
| 2013
| 2.6 y
| 511, 1 275 keV gamma
|
|-
| 4
| Storage 3 #4
| 57Co
| 1
| 37
| 2013
| 272 d
| 122 keV gamma
|
|-
| 5
| Storage 3 #5a
| 60Co
| 1
| 37
| 2005
| 5.3 y
| 1 173, 1 333 keV gamma
|
|-
| 6
| Storage 3 #5b
| 60Co
| 1
| 37
| 2005
| 5.3 y
| 1 173, 1 333 keV gamma
|
|-
| 7
| Storage 3 #6
| 137Cs
| 5
| 185
| 1999
| 30 y
| 662 keV gamma
|
|-
| 8
| Storage 3 #7
| 241Am
| 1
| 37
| 1976
| 458 y
| Alpha + 60 keV gamma
| Glass tube set
|-
| 9
| Storage 3 #8
| 90Sr
| 1
| 37
| 1976
| 29 y
| e-
| Glass tube set
|-
| 10
| Storage 3 #9
| 55Fe
| 10
| 370
| 1976
| 30 y
| 662 keV gamma
| Glass tube set
|-
| 11
| Storage 3 #10
| 106Ru
| 2.7
| 100
| 2000
| 374 d
| e-
|
|-
| 12
| Storage 3 #11
| 241Am
| 10
| 370
| 1975
| 458 y
| Alpha + 60 keV gamma
| ORTEC AM-1U, S/N M-1343, act. 0.088
|-
|}

===Storage 2===
{| class="wikitable"
|-
! Item
! Source ID
! Isotope
! Activity, µCi
! Aktivity, kBq
! Year
! Half-life
! Radiation type
! Note
|-
| 1
| Storage 2 #1a
| 137Cs
| 5
| 185
| 2003
| 30 y
| 662 keV gamma
|
|-
| 2
| Storage 2 #1b
| 137Cs
| 5
| 185
| 2003
| 30 y
| 662 keV gamma
|
|-
| 3
| Storage 2 #1c
| 137Cs
| 5
| 185
| 2003
| 30 y
| 662 keV gamma
|
|-
| 4
| Storage 2 #1d
| 137Cs
| 5
| 185
| 2003
| 30 y
| 662 keV gamma
|
|-
| 5
| Storage 2 #1e
| 137Cs
| 5
| 185
| 2003
| 30 y
| 662 keV gamma
|
|-
| 6
| Storage 2 #1f
| 137Cs
| 5
| 185
| 2003
| 30 y
| 662 keV gamma
|
|-
| 7
| Storage 2 #2
| 137Cs
| 5
| 185
| 1999
| 30 y
| 662 keV gamma
|
|-
| 8
| Storage 2 #3a
| 90Sr
| 0.1
| 3.7
| 2005
| 29 y
| e-
|
|-
| 9
| Storage 2 #3b
| 90Sr
| 0.1
| 3.7
| 2005
| 29 y
| e-
|
|-
| 10
| Storage 2 #4a
| 210Po
| 0.1
| 3.7
| 2005
| 138 d
| 803 keV gamma
|
|-
| 11
| Storage 2 #4b
| 210Po
| 0.1
| 3.7
| 2005
| 138 d
| 803 keV gamma
|
|-
| 12
| Storage 2 #5a
| 137Cs
| 5
| 185
| 1972
| 30 y
| 662 keV gamma
|
|-
| 13
| Storage 2 #5b
| 137Cs
| 5
| 185
| 1972
| 30 y
| 662 keV gamma
|
|-
| 14
| Storage 2 #6
| 60Co
| 5
| 185
| 1972
| 5.3 y
| 1 173, 1 333 keV gamma
|
|-
| 15
| Storage 2 #7
| 152Eu
| 0.04
| 1.5
| 2006
| 13.5 y
| Many gamma lines
| Sealed Liquid
|-
| 16
| Storage 2 #8a
| 22Na
| 1
| 37
| 2005
| 2.6 y
| 511, 1 275 keV gamma
|
|-
| 17
| Storage 2 #8b
| 22Na
| 1
| 37
| 2005
| 2.6 y
| 511, 1 275 keV gamma
|
|-
| 18
| Storage 2 #8c
| 22Na
| 1
| 37
| 2005
| 2.6 y
| 511, 1 275 keV gamma
|
|-
| 19
| Storage 2 #9a
| 137Cs
| 0.5
| 18.5
| 2005
| 30 y
| 662 keV gamma
|
|-
| 20
| Storage 2 #9b
| 137Cs
| 0.5
| 18.5
| 2005
| 30 y
| 662 keV gamma
|
|-
| 21
| Storage 2 #9c
| 137Cs
| 0.5
| 18.5
| 2005
| 30 y
| 662 keV gamma
|
|-
| 22
| Storage 2 #9d
| 137Cs
| 0.5
| 18.5
| 2005
| 30 y
| 662 keV gamma
|
|-
| 23
| Storage 2 #10
| 152Eu
| 1
| 37
| 2005
| 13.5 y
| Many gamma lines
|
|-
| 24
| Storage 2 #11a
| 204Tl
| 10
| 370
| 1993
| 3.78 y
| 511 keV gamma
| Al housing
|-
| 25
| Storage 2 #11b
| 204Tl
| 10
| 370
| 1993
| 3.78 y
| 511 keV gamma
| Al housing
|-
| 26
| Storage 2 #11c
| 204Tl
| 10
| 370
| 1993
| 3.78 y
| 511 keV gamma
| Al housing
|-
| 27
| Storage 2 #11d
| 204Tl
| 10
| 370
| 1993
| 3.78 y
| 511 keV gamma
| Al housing
|-
| 28
| Storage 2 #12a
| 226Ra
| 0.09
| 3.3
| 2005
| 1 600 y
| 186 keV gamma
| Glass jar
|-
| 29
| Storage 2 #12b
| 226Ra
| 0.09
| 3.3
| 2005
| 1 600 y
| 186 keV gamma
| Glass jar
|-
| 30
| Storage 2 #12c
| 226Ra
| 0.09
| 3.3
| 2005
| 1 600 y
| 186 keV gamma
| Glass jar
|-
| 31
| Storage 2 #13
| 241Am
| 0.24
| 9
| N/A
| 458 y
| 60 keV gamma
| GDM 625
|-
| 32
| Storage 2 #14
| 137Cs
| 1.22
| 45
| N/A
| 30 y
| 662 keV gamma
| GDM 134
|-
| 33
| Storage 2 #15
| UO2
| N/A
| N/A
| N/A
| N/A
| N/A
| Nuclear fuel pellet (black cylinder in epoxy cube)
|-
|}

===Storage 1===
====White====
{| class="wikitable"
|-
! Item
! Source ID
! Isotope
! Activity, µCi
! Aktivity, kBq
! Year
! Half-life
! Radiation type
! Note
|-
| 1
| Storage 1W #1
| 241Am
| 10 000
| 370 000
|
| 458 y
| X-rays
| Variable X-ray source
|-
| 2
| Storage 1W #2
| 241Am
| 10
| 370
| 1993
| 458 y
| 60 keV gamma
| DA289 written on the source
|-
| 3
| Storage 1W #3
| 60Co
| 10
| 370
| 1970
| 10.5 y
| 1 173, 1 333 keV gamma
| A943F
|-
| 4
| Storage 1W #4
| 147Pm
| 10 000
| 370 000
| 1974
| 2.6 y
| 76, 198 keV gamma
| A1124/N11958
|-
| 5
| Storage 1W #5
| 137Cs
| 10
| 370
|
| 30 y
| 662 keV gamma
| S/N 15319; A919F
|-
| 6
| Storage 1W #6
| 60Co
| 1
| 37
|
| 10.5 y
| 1 173, 1 333 keV gamma
| S/N 811-L-1
|-
| 7
| Storage 1W #7
| 241Am
| 0.1
| 3.7
| 1966
| 458 y
| 60 keV gamma
| A922F; S/N M954 Ortec
|-
| 8
| Storage 1W #8
| 241Am
| 10 000
| 370 000
| 2010
| 458 y
| 60 keV gamma
|
|-
| 9
| Storage 1W #9
| 137Cs
| 100
| 3 700
| 1984
| 30 y
| 662 keV gamma
|
|-
| 10
| Storage 1W #10
| 241Am
| 14 000
| 518 000
| 1984
| 458 y
| 60 keV gamma
| M55005
|-
| 11
| Storage 1W #11
| 241Am
| 10 000
| 370 000
| 2010
| 458 y
| 60 keV gamma
|
|-
| 12
| Storage 1W #12
| 226Ra
| 5-10
| 185-370
| 1970
| 1 600 y
| 186 keV gamma
| A859F; Leybold in a jar
|-
| 13
| Storage 1W #13
| 137Cs
| <10
| <370
| 2005
| 30 y
| 662 keV gamma
| Isotope generator
|-
| 14
| Storage 1W #14a
| 238U
| 1
| 37
| 2006
| 4.5e9 y
| 50, 114 keV gamma + alpha
| Liquid in plastic bottles (B. Stugu’s)
|-
| 15
| Storage 1W #14b
| 238U
| 1
| 37
| 2006
| 4.5e9 y
| 50, 114 keV gamma + alpha
| Liquid in plastic bottles (B. Stugu’s)
|-
| 16
| Storage 1W #14c
| 238U
| 1
| 37
| 2006
| 4.5e9 y
| 50, 114 keV gamma + alpha
| Liquid in plastic bottles (B. Stugu’s)
|-
| 17
| Storage 1W #15
| 90Sr
| 2 000
| 74 000
| 1987
| 29 y
| e-
| Amersham (in a square Pb collimator)
|-
| 18
| Storage 1W #16
|
|
|
| 1945
|
|
| Hiroshima dust
|-
| 19
|
|
| 0
| 0
| 2005
|
|
| Eluting solution for Tilf #13 Isotope generator
|-
|}
====Black====
{| class="wikitable"
|-
! Item
! Source ID
! Activity, counts/s*
! Note
|-
| 1
| Storage 1B #1
| ~20
| Storage 1B R. 1
|-
| 2
| Storage 1B #2
| ~120
| Storage 1B G. 1
|-
| 3
| Storage 1B #3
| ~60
| Storage 1B G. 2
|-
| 4
| Storage 1B #4
| ~100
| Storage 1B G. 3
|-
| 5
| Storage 1B #5
| ~10
| Storage 1B G. 4
|-
| 6
| Storage 1B #6
| ~10
| Storage 1B G. 5
|-
| 7
| Storage 1B #7
| ~0
| Storage 1B G. 6
|-
| 8
| Storage 1B #8
| ~220
| Storage 1B G. 7
|-
| 9
| Storage 1B #9
| ~150
| Storage 1B G. 8
|-
| 10
| Storage 1B #10
| ~10
| Storage 1B G. 9
|-
| 11
| Storage 1B #11
| ~350
| Storage 1B G. 10
|-
| 12
| Storage 1B #12
| ~500
| Storage 1B G. 11
|-
| 13
| Storage 1B #13
| ~1 000
| Storage 1B G. 12
|-
|}
<nowiki>*</nowiki>Activity measured with an 1" NaI(Tl) crystal

Strålevern

2018-11-16T14:47:23Z

Gge002:

Strålevern

2018-11-16T14:35:40Z

Gge002:

Strålevern

2018-11-16T14:16:48Z

Gge002:

Strålevern

2018-11-16T13:58:24Z

Gge002:

Strålevern

2018-11-16T13:18:15Z

Gge002:

Strålevern

2018-11-16T13:16:44Z

Gge002:

Strålevern

2018-11-16T13:01:23Z

Gge002:

Strålevern

2018-11-16T12:55:19Z

Gge002:

Strålevern

2018-11-16T12:40:18Z

Gge002:

Strålevern

2018-11-16T12:30:18Z

Gge002:

Strålevern

2018-11-16T12:28:41Z

Gge002:

Strålevern

2018-11-16T12:11:07Z

Gge002:

Strålevern

2018-11-16T11:58:34Z

Gge002:

Strålevern

2018-11-16T11:47:10Z

Gge002:

Strålevern

2018-11-16T11:15:13Z

Gge002:

Strålevern

2018-11-16T11:12:06Z

Gge002:

Strålevern

2018-11-16T10:43:39Z

Gge002:

Strålevern

2018-05-29T14:30:34Z

Gge002:

File:Hierarket.jpg

2018-05-29T13:29:58Z

Gge002:

Strålevern

2018-02-26T11:58:36Z

Gge002: /* Regler for bruk av strålekilder på IFT */

==Førstegangsbrukere==
Førstegangsbrukere skal:
#Ta kontakt med strålevernkoordinator (STK)
#Få de nødvendige instruksene fra STK om interne regler for bruk av strålekilder
#Bli registrert for å få personlig dosimeter
#Vente på dosimeteret (tar ca. 1-2 uker)
#Begynne å bruke kilder etter de har fått sitt personlige dosimeter
#Returnere dosimeteret sitt hvis det ikke trengs lenger (gravide brukere skal ikke jobbe med strålingskilder i løpet av svangerskapet)

==Regler for bruk av strålekilder på IFT==
[[File:hierarket.jpg|thumb|alt=Hierarke|Fig. 1 Hierarke]]
[[File:TableHeader.jpg|thumb|alt=Logbokformat|Fig. 2 Logbokformat]]
[[File:Slide2.JPG|thumb|alt=Logbokformat|Fig. 3 Skilt som brukes til svake kilder]]
[[File:Slide1.JPG|thumb|alt=Logbokformat|Fig. 4 Skilt som brukes til sterke kilder og kontaminerte områder hvor begrenset opphold er bare tillatt]]

#Strålevernkoordinatoren (STK) har oversikt over alle kildenes status.
#Ansvarshierarkiet er som vist i Fig. 1.
#Hver lab bør ha lab kildeansvarlig. I tilfelle det ikke er lab-kildeansvarlig deles kildene ut av STK.
#Lab-kildeansvarlig velges av lab-brukerne, STK eller instituttleder.
#Hver lab skal ha loggbok hvor bevegelsene til hver kilde som hører til denne laben skal registreres. Loggboken skal ha formatet som vist i Fig. 2:
#Den første siden i loggboken skal ha navn og kontaktinfo til lab kildeansvarlig og navn og kontakt info til STK.
#Loggboken skal være på labben til enhver tid, bundet med snor til kildeskapet.
#Det er lab kildeansvarlig sitt ansvar å føre boken riktig.
#STK skal kontrollere jobben til lab-kildeansvarlig ofte og uten varsel.
#Det er 1 nøkkel til tilsvarende kildeskap hos lab-kildeansvarlig og 1 nøkkel hos STK. Leder for teknisk Avdeling (TA) og 1 ingeniør fra TA skal kunne få tilgang til STK sine nøkler i tilfelle STK ikke er tilstede.
#Alle personer som har tilgang til nøkler til kildeskap får opplæring i dette regelverket og generell strålevern fra STK.
#Ingen av ovennevnte får lov til å låne sin nøkkel til noen. STK kan delegere ansvaret for nøklene sine, men overføringen skal skje med overtagelsesprotokoll som er en del av loggboken. Lab-kildeansvarlig kan IKKE delegere sitt ansvar for nøkkelen.
#En kildebruker skal først ta kontakt med sin lab-kildeansvarlig. Hvis han/hun ikke er tilstede kontaktes STK. Hvis han/hun ikke er til stedet kontaktes leder TA. Hvis han/hun ikke er til stedet kontaktes ingeniøren som er ansvarlig. Det er IKKE lov å hoppe over noen.
#Hvis lab kildeansvarlig sier opp blir det varetelling med STK og instituttleder og signering av overtagelsesprotokoll.
#Hvis STK sier opp blir det varetelling med UiB STK, instituttleder og den nye STK. Overtagelsesprotokoll signeres.
#Arbeidsplass med åpen strålekilde skal merkeres med skilt (Fig. 3 eller Fig. 4) og eksponeringsvurdering skal utføres.
#Det er ikke ønskelig å la kilder stå uovervåket. Hvis dette er nødvendig skal arbeidstedet markeres.
#Det er ikke lov å jobbe med strålekilder uten dosimeter. STK og HMS-ansvarlig skal kontrollere labbene og brukerne uten varsel.
#Hver bruker skal ha innføring i strålevern fra STK før de begynner å jobbe med kilder. Studenter som har bestått PHYS231 Strålingsfysikk får fritak.
#Gravide brukere skal returnere sine dosimetere til HMS-ansvarlige i det øyeblikket de finner ut at de er gravide (se punkt 18). Dosimeteret blir returnert etter fødsel om det fremdeles er ønskelig.
#Brukere som ikke har bruk for dosimeter lenger skal returnere dem til HMS ansvarlig.
#Dosimetrene skal oppbevares på samme sted når de ikke er i bruk. Det stede skal bestemmes mellom bruker, STK og personen som er ansvarlig for den periodiske skift av TLD.
#De personlige dosimetrene skal brukes bare på IFT og skal ikke taes fra huset. Dette inkluderer ansatte som jobber på eksterne fasiliteter som f.eks. CERN. Sånne ansatte får dosimetrer fra fasilitetene de besøker.

Strålevern

2017-02-16T17:03:20Z

Gge002:

Strålevern

2017-02-16T08:35:54Z

Gge002:

==Førstegangsbrukere==
Førstegangsbrukere skal:
#Ta kontakt med strålevernkoordinator (STK)
#Få de nødvendige instruksene fra STK om interne regler for bruk av strålekilder
#Bli registrert for å få personlig dosimeter
#Vente på dosimeteret (tar ca. 1-2 uker)
#Begynne å bruke kilder etter de har fått sitt personlige dosimeter
#Returnere dosimeteret sitt hvis det ikke trengs lenger (gravide brukere skal ikke ha dosimeter i løpet av svangerskapet)

==Regler for bruk av strålekilder på IFT==
[[File:hierarket.jpg|thumb|alt=Hierarke|Fig. 1 Hierarke]]
[[File:TableHeader.jpg|thumb|alt=Logbokformat|Fig. 2 Logbokformat]]
[[File:Slide2.JPG|thumb|alt=Logbokformat|Fig. 3 Skilt som brukes til svake kilder]]
[[File:Slide1.JPG|thumb|alt=Logbokformat|Fig. 4 Skilt som brukes til sterke kilder og kontaminerte områder hvor begrenset opphold er bare tillatt]]

#Strålevernkoordinatoren (STK) har oversikt over alle kildenes status.
#Ansvarshierarkiet er som vist i Fig. 1.
#Hver lab bør ha lab kildeansvarlig. I tilfelle det ikke er lab-kildeansvarlig deles kildene ut av STK.
#Lab-kildeansvarlig velges av lab-brukerne, STK eller instituttleder.
#Hver lab skal ha loggbok hvor bevegelsene til hver kilde som hører til denne laben skal registreres. Loggboken skal ha formatet som vist i Fig. 2:
#Den første siden i loggboken skal ha navn og kontaktinfo til lab kildeansvarlig og navn og kontakt info til STK.
#Loggboken skal være på labben til enhver tid, bundet med snor til kildeskapet.
#Det er lab kildeansvarlig sitt ansvar å føre boken riktig.
#STK skal kontrollere jobben til lab-kildeansvarlig ofte og uten varsel.
#Det er 1 nøkkel til tilsvarende kildeskap hos lab-kildeansvarlig og 1 nøkkel hos STK. Leder for teknisk Avdeling (TA) og 1 ingeniør fra TA skal kunne få tilgang til STK sine nøkler i tilfelle STK ikke er tilstede.
#Alle personer som har tilgang til nøkler til kildeskap får opplæring i dette regelverket og generell strålevern fra STK.
#Ingen av ovennevnte får lov til å låne sin nøkkel til noen. STK kan delegere ansvaret for nøklene sine, men overføringen skal skje med overtagelsesprotokoll som er en del av loggboken. Lab-kildeansvarlig kan IKKE delegere sitt ansvar for nøkkelen.
#En kildebruker skal først ta kontakt med sin lab-kildeansvarlig. Hvis han/hun ikke er tilstede kontaktes STK. Hvis han/hun ikke er til stedet kontaktes leder TA. Hvis han/hun ikke er til stedet kontaktes ingeniøren som er ansvarlig. Det er IKKE lov å hoppe over noen.
#Hvis lab kildeansvarlig sier opp blir det varetelling med STK og instituttleder og signering av overtagelsesprotokoll.
#Hvis STK sier opp blir det varetelling med UiB STK, instituttleder og den nye STK. Overtagelsesprotokoll signeres.
#Arbeidsplass med åpen strålekilde skal merkeres med skilt (Fig. 3 eller Fig. 4) og eksponeringsvurdering skal utføres.
#Det er ikke ønskelig å la kilder stå uovervåket. Hvis dette er nødvendig skal arbeidstedet markeres.
#Det er ikke lov å jobbe med strålekilder uten dosimeter. STK og HMS-ansvarlig skal kontrollere labbene og brukerne uten varsel.
#Hver bruker skal ha innføring i strålevern fra STK før de begynner å jobbe med kilder. Studenter som har bestått PHYS231 Strålingsfysikk får fritak.
#Gravide brukere skal returnere sine dosimetere til HMS-ansvarlige i det øyeblikket de finner ut at de er gravide (se punkt 18). Dosimeteret blir returnert etter fødsel om det fremdeles er ønskelig.
#Brukere som ikke har bruk for dosimeter lenger skal returnere dem til HMS ansvarlig.
#Dosimetrene skal oppbevares på samme sted når de ikke er i bruk. Det stede skal bestemmes mellom bruker, STK og personen som er ansvarlig for den periodiske skift av TLD.

File:Slide1.JPG

2017-02-16T08:29:57Z

Gge002: File uploaded with MsUpload

File uploaded with MsUpload

File:Slide2.JPG

2017-02-16T08:29:57Z

Gge002: File uploaded with MsUpload

File uploaded with MsUpload

Strålevern

2017-02-16T08:22:50Z

Gge002:

==Førstegangsbrukere==
Førstegangsbrukere skall:
#Ta kontakt med strålevernkoordinator (STK)
#Få de nødvendige instruksene fra STK om interne regler for bruk av strålingskilder
#Bli registrert for å få personlig dosimeter
#Vente på dosimeteret (tar ca. 1-2 uker)
#Begynne å bruke kilder etter de har fått sitt personlige dosimeter
#Returnere dosimeteret sitt hvis det ikke trengs lenger (gravide brukere skal ikke ha dosimeter i løpet av graviditeten)

==Regler for bruk av strålingskilder på IFT==
[[File:hierarket.jpg|thumb|alt=Hierarke|Fig. 1 Hierarke]]
[[File:TableHeader.jpg|thumb|alt=Logbokformat|Fig. 2 Logbokformat]]

#Strålevernkoordinatoren (STK) har oversikt over alle kildenes status.
#Ansvarshierarkiet er som vist i Fig. 1.
#Hver lab bør ha lab kildeansvarlig. I tilfelle det ikke er lab-kildeansvarlig deles kildene ut av STK.
#Lab-kildeansvarlig velges av lab-brukerne, STK eller instituttleder.
#Hver lab skal ha loggbok hvor bevegelsene til hver kilde som hører til denne laben skal registreres. Loggboken skal ha formatet som vist i Fig. 2:
#Den første siden i loggboken skal ha navn og kontaktinfo til lab kildeansvarlig og navn og kontakt info til STK.
#Loggboken skal være på labben til enhver tid, bindet med tråd til kildeskapet.
#Det er lab kildeansvarlig sitt ansvar å føre boken riktig.
#STK skal kontrollere jobben til lab-kildeansvarlig ofte og uten varsel.
#Det er 1 nøkkel til tilsvarende kildeskap hos lab-kildeansvarlig og 1 nøkkel hos STK. Leder for teknisk Avdeling (TA) og 1 ingeniør fra TA skal kunne få tilgang til STK sine nøkler i tilfelle STK ikke er tilstede.
#Alle personer som har tilgang til nøkler til kildeskap får opplæring i dette regelverket og generell strålevern fra STK.
#Ingen av ovennevnte får lov til å låne sin nøkkel til noen. STK kan delegere ansvaret for nøklene sine, men overføringen skal skje med overtagelsesprotokoll som er en del av loggboken. Lab-kildeansvarlig kan IKKE delegere sitt ansvar for nøkkelen.
#En kildebruker skal først ta kontakt med sin lab-kildeansvarlig. Hvis han/hun ikke er tilstede kontaktes STK. Hvis han/hun ikke er til stedet kontaktes leder TA. Hvis han/hun ikke er til stedet kontaktes ingeniøren som er ansvarlig. Det er IKKE lov å hoppe over noen.
#Hvis lab kildeansvarlig sier opp blir det varetelling med STK og instituttleder og signering av overtagelsesprotokoll.
#Hvis STK sier opp blir det varetelling med UiB STK, instituttleder og den nye STK. Overtagelsesprotokoll signeres.
#Arbeidsplass med åpen strålekilde skal merkeres med skilt og eksponeringsvurdering skal utføres.
#Det er ikke ønskelig å la kilder stå uovervåket. Hvis dette er nødvendig skal arbeidstedet markeres.
#Det er ikke lov å jobbe med strålekilder uten dosimeter. STK og HMS-ansvarlig skal kontrollere labbene og brukerne uten varsel.
#Hver bruker skal ha innføring i strålevern fra STK før de begynner å jobbe med kilder. Studenter som har bestått PHYS231 Strålingsfysikk får fritak.
#Gravide brukere skal returnere sine dosimetere til HMS-ansvarlige i det øyeblikket de finner ut at de er gravide (se punkt 18). Dosimeteret blir returnert etter fødsel om det fremdeles er ønskelig.
#Brukere som ikke har bruk for dosimeter lenger skal returnere dem til HMS ansvarlig.

Strålevern

2017-02-15T14:49:29Z

Gge002: Created page with "=Strålevern= ==Førstegangsbrukere== ==Regler for bruk av strålingskilder på IFT== Fig. 1 Hierarke File:TableHeader.jpg|thum..."

=Strålevern=

==Førstegangsbrukere==

==Regler for bruk av strålingskilder på IFT==
[[File:hierarket.jpg|thumb|alt=Hierarke|Fig. 1 Hierarke]]
[[File:TableHeader.jpg|thumb|alt=Logbokformat|Fig. 2 Logbokformat]]

#Strålevernkoordinatoren (STK) har oversikt over alle kildenes status.
#Hierarket er som i Fig. 1.
#Hver lab bør ha lab kildeansvarlig. I tilfelle det ikke er lab kildeansvarlig deles kildene ut av STK.
#Lab kildeansvarlig velges av brukerne til den labben, STK eller Instituttleder.
#Hver lab skal ha logbok hvor bevegelsene av hver kilde som hører til denne laben skal registreres. Logboken skal ha formatet fra Fig. 2:
#Den første siden i labboken skal ha navn og kontaktinfo til lab kildeansvarlig og navn og kontakt info til STK.
#Logboken skal være på labben til enhver tid, bindet med tråd til kildeskapet.
#Det er lab kildeansvarlig sitt ansvar å føre boken riktig.
#STK skal kontrollere jobben til lab kildeansvarlig ofte og uten varsel.
#Det blir 1 nøkler til tilsvarende kildeskap med lab kildeansvarlig og 1 nøkkel med STK. Leder Teknisk Avdeling (TA) og 1 ingeniør fra TA skal kunne få tilgang til STK sine nøkler i tilfelle STK ikke er til stedet.
#Alle personer som har tilgang til nøkler til kildeskap får opplæring i dette regelverket og generell strålevern fra STK.
#Ingen av overnevnte får lov til å låne sin nøkkel til noen. STK kan delegere ansvaret for nøklene sine men overføringen skal skje med overtagelsesprotokoll som er en del av logboken. Lab kildeansvarlig kan IKKE delegere sitt ansvar for nøkkelen.
#En kildebruker skal først ta kontakt med sin lab kildeansvarlig. Hvis han/hun ikke er til stedet kontaktes STK. Hvis han/hun ikke er til stedet kontaktes leder TA. Hvis han/hun ikke er til stedet kontaktes ingeniøren som er ansvarlig. Det er IKKE lov å hoppe over hodet på noen.
#Hvis lab kildeansvarlig sier opp blir det varetelling med STK og instituttleder og signering av overtagelsesprotokoll.
#Hvis STK sier opp blir det varetelling med UiB STK, instituttleder og den nye STK. Overtagelsesprotokoll signeres.
#Arbeidsplass med åpen strålingskilde skal markeres med skilt og eksponeringsvurdering skal utføres.
#Det er ikke ønskelig å la kilder stå uovervåket. Hvis dette er nødvendig skal arbeidstedet markeres.
#Det er ikke lov å jobbe med strålingskilder uten dosimeter. STK og HMS ansvarlig skal kontrollere labbene og brukerne uten varsel.
#Hver bruker skal ha innføring i strålevern fra STK før de begynner å jobbe med kilder. Studenter som har bestått PHYS231 Strålingsfysikk får fritak.
#Gravide brukere skal returnere sine dosimetrer til HMS ansvarlig i øyeblikket de finner ut at de er gravide (se punkt 18). Dosimetrene blir returnert etter fødsel om fremdeles ønskelig.
#Brukere som ikke har bruk for dosimeter lenger skal returnere dem til HMS ansvarlig.

File:TableHeader.jpg

2017-02-15T14:33:09Z

Gge002: File uploaded with MsUpload

File uploaded with MsUpload

Main Page

2017-02-15T14:26:11Z

Gge002:

=Velkommen til [http://www.uib.no/ift Institutt for Fysikk og Teknologis]Wiki=

* [[DAMARA]]
* [[Detector lab]]
* [[Eksperimentalfysikk med prosjektoppgave - PHYS117]]
* [[Experimental Nuclear Physics group]]
* [[Microelectronics group]]
* [http://wiki.uib.no/nanolab Nano Lab]
* [[Particle Physics group]]
* [[Strålevern]]
* [[Teknisk avdeling]]

== Komme i gang ==

* [[Få tilgang til å opprette eller redigere sider i wikien]]
* [http://meta.wikimedia.org/wiki/Help:Contents User's Guide]
* [http://www.mediawiki.org/wiki/Manual:FAQ MediaWiki FAQ]
* [http://lists.wikimedia.org/mailman/listinfo/mediawiki-announce MediaWiki release mailing list]

Bore hole probe

2013-10-04T11:35:06Z

Gge002:

==Project description==
In this project, radioactivity measurements will be performed in several Boreholes around Bergen region. Boreholes are drilled to provide thermal energy coming from hot underground water that is used to heat buildings. The goal of this project is to perform radioactivity measurements as a function of depth in Boreholes. The radioactivity will be monitored by means of a Geiger-Muller (GM) counter (Figure 1 shows the details of the detector to be utilized in this work). This is a gas-filled, cylindrical radiation counter that has found many industrial applications such as level gauges in the oil and gas industry. This is primarily due to the GM counter's robustness, low cost, simple read-out electronics and insensitivity to pressure and temperature changes in the environment. GM counters are also relatively insensitive to mechanical vibrations. These properties of the counter make it a good alternative for the pertinent measurements, as these will be carried out at varying depths in the boreholes. The counter will need to be lowered down as deep as 300 m. In order to carry out measurements across very long cables, there will be a need for a special detector data acquisition (DAQ) system, which includes electronic micro-controller, amplifier, pulse inverter, and hardware control programming. The project will start by designing the aforementioned DAQ system. Following a successful design, the system will be fabricated/built and tested. Once this is ready one can start measuring activities in Boreholes around the Bergen area.

Students who are interested in radiation detection and detector readout electronics are very welcome.
==Supervisors==
Prof. Dr. Bjarne Stugu

Dr. Ilker Meric

Dr. Enver Alagoz

==GM counter==
[[File:GM_tube2.jpg|200px|thumb|right|Figure 1. Cross-sectional view of the ZP1200 GM counter. All dimensions are given in mm.]]
[[File:GMtube.jpg|200px|thumb|right|Figure 2. ZP1200 circuitry]]
The GM counter for this project is ZP1200. This is a Na-Halogen filled GM with a 446 stainless steel cathode. Its effective length is 38.1 mm. Operates in the temperature range from -40°C to +75°C. It has a max starting voltage of 325 V, an operating voltage range from 450 V to 650 V, recommended operating voltage of 500 V and a max slope of the plateau 6%/100V. The dead time of the detector is minimum 90 µs. It weighs 8 g.

File:GM tube2.jpg

2013-10-04T11:20:46Z

Gge002:

Bore hole probe

2013-10-03T09:50:00Z

Gge002: Created page with "==GM counter== ZP1200 circuitry The GM counter for this project is ZP1200."

==GM counter==
[[File:GMtube.jpg|200px|thumb|right|ZP1200 circuitry]]
The GM counter for this project is ZP1200.

File:GMtube.jpg

2013-10-03T09:45:07Z

Gge002:

Eksperimentalfysikk med prosjektoppgave - PHYS117

2013-10-03T09:35:57Z

Gge002:

==Projects==
* [[Applied Planetary Radio Astronomy]]
* [[Phys117_-_PET_project|PET detector]]
* [[Bore hole probe]]

==Useful stuff==
* [[Inductance_meter|Inductance meter]]

Inductance meter

2013-10-03T08:15:14Z

Gge002:

==Objective==
A traditional multimeter accessible to the hobbyist can measure all essential electric properties, including capacitance. The only property that still remains difficult to measure without extra investments (which can become rather significant) is inductance.
Solenoids/coils are an essential part of any analogue circuit and, as opposed to all other discrete components, are often homemade. There are formulae helping to calculate parameters like number of windings, cross-section of the core and so on for a desired inductance to be obtained, but one critically needs to verify the inductance of the final product. This article describes how one can build a rather accurate L-meter at home for probably less than $10. Here you will find the schematic, PCB layout, micro-controller source code; basically all you need to DIY.

==Description==
The L-meter presented here is based on a rather popular solution using the LM311 comparator (see e.g. [http://electronics-diy.com/lc_meter.php]). It is stripped from the capacitance measuring capability due to micro-controller unit (MCU) source code size limitation. This limitation is dictated by the compiler I have used: MikroC PRO for PIC, ver. 6.0.0, not the MCU itself. The free license of the compiler allows up to 2k of program words (2066 to be exact, and the present code is 2065 program words).

Other solutions omitting the LM311 and using built-in the MCU comparators can also be found (see e.g. [https://sites.google.com/site/vk3bhr/home/index2-html]).

The MCU used in this project is PIC 16F88. The code given below is also for this MCU. The internal oscillator block is used, working at 4 MHz (selected by the OSCCON register, bits 6-4). The prescaler is set to 1:1 on the watchdog timer (OPTION_REG register, bits 2-0).

==Specs==
The L-meter presented here has a lower limit of ~1 µH and an upper limit of ~1 MH (Mega Henry).

Some sources (e.g. [http://electronics-diy.com/lc_meter.php]) claim lower limits as low as 10 nH, but I personally do not see how this can be achieved with the current solution. For more details see section "Theory and Schematic".

Power source: 6-24 VDC adapter.

==Theory and Schematic==
[[File:ChestotomerShema.png|600px|thumb|right|L-meter schematic (Erratum: J1 should receive more than 6 VDC and less than 24 VDC, not 5 VDC as in the schematic)]]
The working principle of the schematic is as follows:
* A tank circuit consisting of the capacitor C3 and the unknown coil (Lx) will oscillate at a resonance frequency:

<math>f = \frac{1}{2\pi\sqrt{LC}}</math>

The schematic here is designed to work as a frequency counter, counting the frequency of oscillation of the aforementioned tank cirquit LxC3. Then if the value of C3 is known the MCU can measure the frequency, calculate Lx and display it on the LCD:

<math>L = (\frac{1}{2\pi f \sqrt{C}})^2</math>

* Without Lx connected, LM311 works as a free running multivibrator with a frequency on pin 7 ~1 Hz. When some Lx is connected, pin 7 on LM311 starts oscillating with the frequency of the tank cirquit. The bigger Lx the lower the frequency. Thus the upper limit of measurement will be limited by the frequency of the free running multivibrator (~1 Hz) and is therefore of the order of 1 MH.
* The rectangular pulses generated by LM311 will then be picked by the MCU, the frequency and inductance calculated and the inductance displayed on the LCD.

Since the primary measured quantity in this project is frequency, we need to count pulses per unit time. Therefore using some kind of a counter mode of the MCU should be in order. PIC 16F88 has such a mode, as a good deal of the other PIC MCUs. This mode is selected in the OPTION_REG register (TOCS bit). When counter mode is selected, Timer0 counts the external clock pulses on RA4/AN4/T0CKI/C2OUT pin (pin 3). The timer/counter can be set to increment either on the rising or on the falling edge of every pulse arriving at RA4/AN4/T0CKI/C2OUT. This is firmware selectable by the T0SE (Timer0 Source Edge) bit of OPTION_REG. The counting range of the counter can be extended by the use of the prescaler or in the firmware. The latter technically does not increase the range of the counter as such, but it allows reaching very high counts. In the code below the latter method is used, since we are interested in counting every single pulse. Using a prescaler would cause inability to measure lower frequencies.

In theory, if the oscillator frequency is 4 MHz (Tosc 0.25 μs), one cycle will be 4 x Tosc = 1 μs. An external clock signal going directly into the counter (pin RA4/AN4/T0CKI/C2OUT), without prescaler, should be high for longer than 2 x Tosc + 20 = 520 ns and low for at least the same time. This gives a total period of 1040 ns. Thus, the maximum input frequeny is 1/1040 ns = 961.5 KHz. If the prescaler is applied, according to the specs of PIC 16F88 the external clock input must be high/low for more than 10 ns. Consequently, the maximum countable frequency on pin RA4/AN4/T0CKI/C2OUT is 50 MHz. This would give a minimum measurable inductance ~10 nH. Why are we getting only 1 µH then? All boils down to the quality of the pulses LM311 in this configuration can give. The rising edge of these pulses has a relatively poor time constant, which results in a relatively slow saturation. Therefore, if the frequency is high enough the pulse will start falling before the rising edge has reached saturation, thus creating a train of jigsaw shaped pulses with an amplitude decreasing with the increase of the frequency, rather than rectangular ones. And for frequencies higher than what Lx < 33 µH can give the pulse becomes so bad that the MCU cannot correctly interpret it. How can one go from 33 µH down to 1 µH for the minimum inductance measurement then? In the prototype I built the critical Lx is 33 µH. Below this inductance the counter begins to generate more or less random numbers. But if one doesn't know that these are random numbers one might take them for real. Here L1 enters the picture. Whenever an unknown inductor is measured, it will be connected in series with L1 (added to it). Thus, at least 33 µH will always be measured and the system will never get into the region of instability due to bad pulse shape. Then an offset of -33 µH is added in the firmware so that if the Lx input is short circuited 0 µH will be displayed. Now when a 1 µH coil is measured, the display will show 1 µH.

If smaller inductances are to be measured the multivibrator part needs to be redesigned, so that correctly shaped pulses are formed at higher frequencies.

==Layouts==

==Bill of materials==

==Code==

Inductance meter

2013-10-03T07:55:16Z

Gge002:

==Objective==
A traditional multimeter accessible to the hobbyist can measure all essential electric properties, including capacitance. The only property that still remains difficult to measure without extra investments (which can become rather essential) is inductance.
Solenoids/coils are a significant part of any analogue circuit and, as opposed to all other discrete components, are often homemade. There are formulae helping to calculate parameters like number of windings, cross-section of the core etc, but one critically needs to verify the inductance of the final product. This article describes how one can build a rather accurate L-meter at home for probably less than $10. Here you will find the schematic, PCB layout, micro-controller source code; basically all you need to DIY.

==Description==
The L-meter presented here is based on a rather popular solution using the LM311 comparator (see e.g. [http://electronics-diy.com/lc_meter.php]). It is stripped from the capacitance measuring capability due to micro-controller unit (MCU) source code size limitation. This limitation is dictated by the compiler I have used: MikroC PRO for PIC, ver. 6.0.0, not the MCU itself. The free license of the compiler allows up to 2k of program words (2066 to be exact, and the present code is 2065 program words).

Other solutions omitting the LM311 and using built-in the MCU comparators can also be found (see e.g. [https://sites.google.com/site/vk3bhr/home/index2-html]).

The MCU used in this project is PIC 16F88. The code given below is also for this MCU. The internal oscillator block is used, working at 4 MHz (selected by the OSCCON register, bits 6-4). The prescaler is set to 1:1 on the watchdog timer (OPTION_REG register, bits 2-0).

==Specs==
The L-meter presented here has a lower limit of ~1 µH and an upper limit of ~1 MH (Mega Henry).

Some sources (e.g. [http://electronics-diy.com/lc_meter.php]) claim lower limits as low as 10 nH, but I personally do not see how this can be achieved with the current solution. For more details see section "Theory and Schematic".

Power source: 6-24 VDC adapter.

==Theory and Schematic==
[[File:ChestotomerShema.png|600px|thumb|right|L-meter schematic (Erratum: J1 should receive more than 6 VDC and less than 24 VDC, not 5 VDC as in the schematic)]]
The working principle of the schematic is as follows:
* A tank circuit consisting of the capacitor C3 and the unknown coil (Lx) will oscillate at a resonance frequency:

<math>f = \frac{1}{2\pi\sqrt{LC}}</math>

The schematic here is designed to work as a frequency counter, counting the frequency of oscillation of the aforementioned tank cirquit LxC3. Then if we know the value of C3 we can make the MCU measure the frequency, calculate Lx and display it on the LCD:

<math>L = (\frac{1}{2\pi f \sqrt{C}})^2</math>

* Without Lx connected, LM311 works as a free running multivibrator with a frequency on pin 7 ~1 Hz. When some Lx is connected, pin 7 on LM311 starts oscillating with the frequency of the tank cirquit. The bigger Lx the lower the frequency. Thus the upper limit of measurement will be limited by the frequency of the free running multivibrator (~1 Hz) and is therefore ~1 MH.
* The rectangular pulses generated by LM311 will then be picked by the MCU, the frequency and inductance calculated and the inductance displayed on the LCD.

Since the primary measured quantity in this project is frequency, we need to count pulses per unit time. Therefore using some kind of a counter mode of the MCU should be in order. PIC 16F88 has such a mode, as a good deal of the other PIC MCUs. This mode is selected in the OPTION_REG register (TOCS bit). When counter mode is selected, Timer0 counts the external clock pulses on RA4/AN4/T0CKI/C2OUT pin (pin 3). The timer/counter can be set to increment either on the rising or on the falling edge of every pulse arriving at RA4/AN4/T0CKI/C2OUT. This is software selectable by the T0SE (Timer0 Source Edge) bit of OPTION_REG. The counting range of the counter can be extended by the use of the prescaler or in the software. The latter technically does not increase the range of the counter, but it allows reaching very high counts. In the code below the latter method is used, since we are interested in counting every single pulse. Using a prescaler would cause inability to measure lower frequencies.

In theory, if the oscillator frequency is 4 MHz (Tosc 0.25 μs), one cycle will be 4 x Tosc = 1 μs. An external clock signal going directly into the counter (pin RA4/AN4/T0CKI/C2OUT), without prescaler, should be high for longer than 2 x Tosc + 20 = 520 ns and low for at least the same time. This gives a total period of 1040 ns. Thus, the maximum input frequeny is 1/1040 ns = 961.5 KHz. If the prescaler is applied, according to the specs of PIC 16F88 the external clock input must be high/low for more than 10 ns. Consequently, the maximum countable frequency on pin RA4/AN4/T0CKI/C2OUT is 50 MHz. This would give a minimum measurable inductance ~10 nH. Why are we getting only 1 µH then? All boils down to the quality of the pulses LM311 in this configuration can give. The rising edge of these pulses has a relatively poor time constant, which results in a relatively slow saturation. Therefore, if the frequency is high enough the pulse will start falling before the rising edge has reached saturation, thus creating a train of jigsaw shaped pulses with an amplitude decreasing with the increase of the frequency, rather than rectangular ones. And for frequencies higher than what Lx < 33 µH the pulse becomes so bad that the MCU cannot correctly interpret it. How can one go from 33 µH down to 1 µH for the minimum inductance measurement then? In the prototype I built the critical Lx is 33 µH. Below this inductance the counter begins to generate more or less random numbers. But if one doesn't know that these are random numbers one might take them for real. Here L1 enters the picture. Whenever an unknown inductor is measured, it will be connected in series with L1 (added to it). Thus one will always measure at least 33 µH and will never get into the region of instability due to bad pulse shape. One adds to the code in the MCU an offset of -33 µH so that if one shortcircuits the Lx input one will measure 0 µH. Now when one measures a 1 µH coil, the display will show 1 µH.

If one wants to measure smaller inductances one needs to redesign the multivibrator part so that correctly shaped pulses are formed at higher frequencies.

==Layouts==

==Bill of materials==

==Code==

Inductance meter

2013-10-02T14:32:22Z

Gge002:

==Objective==
A traditional multimeter accessible to the hobbyist can measure all essential electric properties, including capacitance. The only property that still remains difficult to measure without extra investments (which can become rather essential) is inductance.
Solenoids/coils are a significant part of any analogue circuit and, as opposed to all other discrete components, are often homemade. There are formulae helping to calculate parameters like number of windings, cross-section of the core etc, but one critically needs to verify the inductance of the final product. This article describes how one can build a rather accurate L-meter at home for probably less than $10. Here you will find the schematic, PCB layout, micro-controller source code; basically all you need to DIY.

==Description==
The L-meter presented here is based on a rather popular solution using the LM311 comparator (see e.g. [http://electronics-diy.com/lc_meter.php]). It is stripped from the capacitance measuring capability due to micro-controller (MCU) source code size limitation. This limitation is dictated by the compiler I have used: MikroC PRO for PIC, ver. 6.0.0. The free license of the compiler allows up to 2k of program words (2066 to be exact, and the present code is 2065 program words).

Other solutions omitting the LM311 and using built-in the MCU comparators can also be found (see e.g. [https://sites.google.com/site/vk3bhr/home/index2-html]).

The MCU used in this project is PIC 16F88. Obviously, the code given below is also for this MCU.

==Specs==
The L-meter presented here has a lower limit of ~1 µH and an upper limit of ~1 MH (Mega Henry).

Some sources (e.g. [http://electronics-diy.com/lc_meter.php]) claim lower limits as low as 10 nH, but I personally do not see how this can be achieved with the current solution. For more details see section "Theory and Schematic".

==Theory and Schematic==
[[File:ChestotomerShema.png|400px|thumb|right|L-meter schematic]]
The working principle of the schematic is as follows:
# A tank circuit consisting of the capacitor C3 and the unknown coil (Lx) will oscillate at a resonance frequency:

<math>f = \frac{1}{2\pi\sqrt{LC}}</math>

The schematic here is designed to work as a frequency counter, counting the frequency of oscillation of the aforementioned tank cirquit LxC3. Then if we know the value of C3 we can make the MCU measure the frequency, calculate Lx and display it on the LCD:

<math>L = (\frac{1}{2\pi f \sqrt{C}})^2</math>

# Without Lx connected, LM311 works as a free running multivibrator with a frequency on pin 7 ~1 Hz. When some Lx is connected, pin 7 on LM311 starts oscillating with the frequency of the tank cirquit. The bigger Lx the lower the frequency. Thus the upper limit of measurement will be limited by the frequency of the free running multivibrator (~1 Hz) and is therefore ~1 MH.
# The rectangular pulses generated by LM311 will then be picked by the MCU, the frequency and inductance calculated and the inductance displayed on the LCD.

In theory if the main oscillator frequency is 4 MHz (Tosc 0.25 μs), one cycle will be 4 x Tosc = 1 μs. An external clock signal going directly into the counter (pin T0CKI), without prescaler, should be high for longer than 2 x Tosc + 20 = 520 ns and low for at least the same time. This gives a total period of 1040 ns. Thus, the maximum input frequeny is 1/1040 ns = 961.5 KHz. If the prescaler is applied, according to the specs of PIC 16F88 the external clock input must be high/low for more than 10 ns. Consequently, the maximum countable frequency on pin T0CKI is 50 MHz. This would give a minimum measurable inductance ~10 nH. Why are we getting only 1 µH then? All boils down to the quality of the pulses LM311 in this configuration can give. The rising edge of these pulses has a relatively poor time constant, which results in a relatively slow saturation. Therefore, if the frequency is high enough the pulse will start falling before the rising edge has reached saturation, thus creating a train of jigsaw shaped pulses with an amplitude decreasing with the increase of the frequency, rather than rectangular ones. And for frequencies higher than what Lx < 33 µH the pulse becomes so bad that the MCU cannot correctly interpret it. How can one go from 33 µH down to 1 µH for the minimum inductance measurement then? In the prototype I built the critical Lx is 33 µH. Below this inductance the counter begins to generate more or less random numbers. But if one doesn't know that these are random numbers one might take them for real. Here L1 enters the picture. Whenever an unknown inductor is measured, it will be connected in series with L1 (added to it). Thus one will always measure at least 33 µH and will never get into the region of instability due to bad pulse shape. One adds to the code in the MCU an offset of -33 µH so that if one shortcircuits the Lx input one will measure 0 µH. Now when one measures a 1 µH coil, the display will show 1 µH.
If one wants to measure smaller inductances one needs to redesign the multivibrator part.

==Layouts==

==Bill of materials==

==Code==

Inductance meter

2013-09-30T20:44:35Z

Gge002:

File:ChestotomerShema.png

2013-09-30T17:00:40Z

Gge002: Gge002 uploaded a new version of "File:ChestotomerShema.png"

File:ChestotomerShema.png

2013-09-30T16:52:30Z

Gge002:

Inductance meter

2013-09-30T16:50:37Z

Gge002: Created page with "==Objective== A traditional multimeter accessible to the hobbyist can measure all essential electric properties, including capacitance. The only property that still remains di..."

Eksperimentalfysikk med prosjektoppgave - PHYS117

2013-09-30T14:47:30Z

Gge002:

==Projects==
* [[Applied Planetary Radio Astronomy]]
* [[Phys117_-_PET_project|PET detector]]

==Useful stuff==
* [[Inductance_meter|Inductance meter]]

Applied Planetary Radio Astronomy

2011-09-28T08:08:48Z

Gge002:

= Jovian Radio Storms =
== Project Outline ==
[[File:Jupiter1.jpg|thumb|alt=Charged partical trajectory in Jupiter's magnetic field|Charged partical trajectory in Jupiter's magnetic field]]
[[File:Jupiter2.jpg|thumb|alt=Origin of the different frequency emissions in Jupiter's magnetic field|Origin of the different frequency emissions in Jupiter's magnetic field]]
[[File:Jupiter3.jpg|thumb|alt=Jupiter's A-, B- and C type radio burst|Jupiter's A-, B- and C type radio burst]]

The project is suitable for 1-2 practically oriented students with broad interests, who do not mind “getting their hands dirty” every now and then, in addition to the time spent in front of the PC.
#Contact persons – Georgi Genov, Kjetil Ullaland, Nikolai Østgaard, Kjell Aarsnes
#Aim - To learn basic radio astronomy, to modify an existing radio telescope amplifier (RTA), to build the telescope’s antennas and to establish observational procedures.
#Tasks
#*Modifying the existing RTA for automatic sweep of the frequency range;
#*Building the electronics required to establish the computer communication;
#*Building and set up of the antennas of the radio telescope;
#*Developing a simple software for data acquisition and preliminary data analysis;
#*Performing tests and developing observational procedures.
#Benefits – learn basic radio astronomy; get hands-on experience with applied electronics, data acquisition and data analysis, development of software for scientific purposes.
#Background
Two types of radio noise emitted by Jupiter have been detected – synchrotron and cyclotron. The latter is strong enough to be detected by small antennas on Earth’s surface. Charged particles spiraling around Jupiter’s magnetic field lines near both magnetic poles (top figure) produce this cyclotron radiation. These shortwave signals are often referred to as DAM, since they fall in the decameter wavelength range. At these higher latitudes, where Jupiter’s magnetic field reaches as far out as Io, its field lines sweep rapidly past the ions and electrons shed into Io’s torus. This induces DAM radiation along the surface of the cyclotron cone (given in magenta in the middle figure). Jupiter’s DAM frequency reaches a maximum of 39.5 MHz near Jupiter’s cloud tops. At twice Jupiter’s radius the frequency is 3 MHz. Intermediate frequencies are created between these two extreme distances. Jupiter radiates two distinctive types of radio signatures in the DAM frequency range:
*L-bursts –long duration static sounding like the swoosh of the waves;
*S-bursts – short duration static resembling the crackling of a campfire.
DAM radiation originates from at least 3 sources (A, B and C) that are fixed with respect to the planet’s rotating magnetic field. These sources are observed at around 20 MHz. They fall largely around one hemisphere (bottom figure). Source A is more than twice more likely to emit than either B or C. Jupiter’s magnetic storms depend on a combination of Io’s orbital position and the inclination of the respective radio source with respect to Earth.

== Original Radio JOVE Project ==
# JOVE Receiver Documentation
# JOVE Antenna Documentation
= Receivers - Construction and Theory =
= Antennae - Construction and Theory =
* [[:File:ParaboloidConcentrator.pdf|How to build a parabolic concentrator]]
= Books =
== The Radio Sky and How to Observe It - by Jeff Lashley ==
Preface and Table of contents

Chapter 1 - The Radio Sun

Chapter 2 - Jupiter

Chapter 3 - Meteors and Meteor Streams

Chapter 4 - Beyond the Solar System

Chapter 5 - Antennae

Chapter 6 - Setting Up a Radio Astronomy Station

Chapter 7 - Radio Hardware Theory

Chapter 8 - Introduction to RF Electronics

Chapter 9 - Building a Very Low Frequency Solar Flare Monitor

Chapter 10 - Microwave Radio Telescope Projects

Chapter 11 - Building a Jupiter Radio Telescope

Chapter 12 - Building a Broad Band Solar Radio Telescope

Chapter 13 - Data Logging and Data Processing

Appendices - Formulae; Bibliography; Suppliers, Groups, and Societies; Glossary

= Articles =
= Miscellaneous =
== Radio Frequency Bands ==

{| class="wikitable", border = '1'
|-style="background: silver"
! Band name
! Abbreviation
! Frequency
! Wavelength
! Usage
|-
|
|
| < 3 Hz
| > 100 000 km
| Natural and man-made electromagnetic noise
|-
| Extremely low frequency
| ELF
| 3 - 30 Hz
| 100 000 - 10 000 km
| Submarine communication
|-
| Super low frequency
| SLF
| 30 - 300 Hz
| 10 000 - 1 000 km
| Submarine communication
|-
| Ultra low frequency
| ULF
| 300 Hz - 3 kHz
| 1 000 - 100 km
| Submarine communication, Communication within mines
|-
| Very low frequency
| VLF
| 3 - 30 kHz
| 100 - 10 km
| Navigation, time signals, submarine communication, wireless heart rate monitors, geophysics
|-
| Low frequency
| LF
| 30 - 300 kHz
| 10 - 1 km
| Navigation, time signals, AM longwave broadcasting (Europe and parts of Asia), RFID, amateur radio
|-
| Medium frequency
| MF
| 300 kHz - 3 MHz
| 1 km - 100 m
| AM medium-wave broadcasts, amateur radio, avalanche beacons
|-
| High frequency
| HF
| 3 - 30 MHz
| 100 m - 10 m
| Shortwave broadcasts, citizens' band radio, amateur radio and over-the-horizon aviation communications, RFID, Over-the-horizon radar, Automatic link establishment (ALE) / Near Vertical Incidence Skywave (NVIS) radio communications, Marine and mobile radio telephony
|-
| Very high frequency
| VHF
| 30 - 300 MHz
| 10 - 1 m
| FM, television broadcasts and line-of-sight ground-to-aircraft and aircraft-to-aircraft communications. Land Mobile and Maritime Mobile communications, amateur radio, weather radio
|-
| Ultra high frequency
| UHF
| 300 MHz - 3 GHz
| 1 m - 100 mm
| Television broadcasts, microwave ovens, microwave devices/communications, mobile phones, wireless LAN, Bluetooth, ZigBee, GPS and two-way radios such as Land Mobile, FRS and GMRS radios, amateur radio
|-
| Super high frequency
| SHF
| 3 - 30 GHz
| 100 - 10 mm
| Microwave devices/communications, wireless LAN, most modern radars, communications satellites, satellite television broadcasting, DBS, amateur radio
|-
| Extremely high frequency
| EHF
| 30 - 300 GHz
| 10 - 1 mm
| High-frequency microwave radio relay, microwave remote sensing, amateur radio, directed-energy weapon, millimeter wave scanner
|-
| Terahertz or Tremendously high frequency
| THz or THF
| 300 GHz - 3 THz
| 1 - 0.1 mm
| Terahertz imaging, ultrafast molecular dynamics, condensed-matter physics, terahertz time-domain spectroscopy, terahertz computing/communications, sub-mm remote sensing, amateur radio
|}

Applied Planetary Radio Astronomy

2011-09-22T17:31:21Z

Gge002: radio freq bands added

= Jovian Radio Storms =
== Project Outline ==
[[File:Jupiter1.jpg|thumb|alt=Charged partical trajectory in Jupiter's magnetic field|Charged partical trajectory in Jupiter's magnetic field]]
[[File:Jupiter2.jpg|thumb|alt=Origin of the different frequency emissions in Jupiter's magnetic field|Origin of the different frequency emissions in Jupiter's magnetic field]]
[[File:Jupiter3.jpg|thumb|alt=Jupiter's A-, B- and C type radio burst|Jupiter's A-, B- and C type radio burst]]

The project is suitable for 1-2 practically oriented students with broad interests, who do not mind “getting their hands dirty” every now and then, in addition to the time spent in front of the PC.
#Contact persons – Georgi Genov, Kjetil Ullaland, Nikolai Østgaard, Kjell Aarsnes
#Aim - To learn basic radio astronomy, to modify an existing radio telescope amplifier (RTA), to build the telescope’s antennas and to establish observational procedures.
#Tasks
#*Modifying the existing RTA for automatic sweep of the frequency range;
#*Building the electronics required to establish the computer communication;
#*Building and set up of the antennas of the radio telescope;
#*Developing a simple software for data acquisition and preliminary data analysis;
#*Performing tests and developing observational procedures.
#Benefits – learn basic radio astronomy; get hands-on experience with applied electronics, data acquisition and data analysis, development of software for scientific purposes.
#Background
Two types of radio noise emitted by Jupiter have been detected – synchrotron and cyclotron. The latter is strong enough to be detected by small antennas on Earth’s surface. Charged particles spiraling around Jupiter’s magnetic field lines near both magnetic poles (top figure) produce this cyclotron radiation. These shortwave signals are often referred to as DAM, since they fall in the decameter wavelength range. At these higher latitudes, where Jupiter’s magnetic field reaches as far out as Io, its field lines sweep rapidly past the ions and electrons shed into Io’s torus. This induces DAM radiation along the surface of the cyclotron cone (given in magenta in the middle figure). Jupiter’s DAM frequency reaches a maximum of 39.5 MHz near Jupiter’s cloud tops. At twice Jupiter’s radius the frequency is 3 MHz. Intermediate frequencies are created between these two extreme distances. Jupiter radiates two distinctive types of radio signatures in the DAM frequency range:
*L-bursts –long duration static sounding like the swoosh of the waves;
*S-bursts – short duration static resembling the crackling of a campfire.
DAM radiation originates from at least 3 sources (A, B and C) that are fixed with respect to the planet’s rotating magnetic field. These sources are observed at around 20 MHz. They fall largely around one hemisphere (bottom figure). Source A is more than twice more likely to emit than either B or C. Jupiter’s magnetic storms depend on a combination of Io’s orbital position and the inclination of the respective radio source with respect to Earth.

== Original Radio JOVE Project ==
# JOVE Receiver Documentation
# JOVE Antenna Documentation
= Receivers - Construction and Theory =
= Antennae - Construction and Theory =
* [[:File:ParaboloidConcentrator.pdf|How to build a parabolic concentrator]]
= Books =
== The Radio Sky and How to Observe It - by Jeff Lashley ==
[[:File:Ch0.pdf|Preface and Table of contents]]

[[:File:Ch1.pdf|Chapter 1 - The Radio Sun]]

[[:File:Ch2.pdf|Chapter 2 - Jupiter]]

[[:File:Ch3.pdf|Chapter 3 - Meteors and Meteor Streams]]

[[:File:Ch4.pdf|Chapter 4 - Beyond the Solar System]]

[[:File:Ch5.pdf|Chapter 5 - Antennae]]

[[:File:Ch6.pdf|Chapter 6 - Setting Up a Radio Astronomy Station]]

[[:File:Ch7.pdf|Chapter 7 - Radio Hardware Theory]]

[[:File:Ch8.pdf|Chapter 8 - Introduction to RF Electronics]]

[[:File:Ch9.pdf|Chapter 9 - Building a Very Low Frequency Solar Flare Monitor]]

[[:File:Ch10.pdf|Chapter 10 - Microwave Radio Telescope Projects]]

[[:File:Ch11.pdf|Chapter 11 - Building a Jupiter Radio Telescope]]

[[:File:Ch12.pdf|Chapter 12 - Building a Broad Band Solar Radio Telescope]]

[[:File:Ch13.pdf|Chapter 13 - Data Logging and Data Processing]]

[[:File:AppA.pdf|Appendices - Formulae; Bibliography; Suppliers, Groups, and Societies; Glossary]]

= Articles =
= Miscellaneous =
== Radio Frequency Bands ==

{| class="wikitable", border = '1'
|-style="background: silver"
! Band name
! Abbreviation
! Frequency
! Wavelength
! Usage
|-
|
|
| < 3 Hz
| > 100 000 km
| Natural and man-made electromagnetic noise
|-
| Extremely low frequency
| ELF
| 3 - 30 Hz
| 100 000 - 10 000 km
| Submarine communication
|-
| Super low frequency
| SLF
| 30 - 300 Hz
| 10 000 - 1 000 km
| Submarine communication
|-
| Ultra low frequency
| ULF
| 300 Hz - 3 kHz
| 1 000 - 100 km
| Submarine communication, Communication within mines
|-
| Very low frequency
| VLF
| 3 - 30 kHz
| 100 - 10 km
| Navigation, time signals, submarine communication, wireless heart rate monitors, geophysics
|-
| Low frequency
| LF
| 30 - 300 kHz
| 10 - 1 km
| Navigation, time signals, AM longwave broadcasting (Europe and parts of Asia), RFID, amateur radio
|-
| Medium frequency
| MF
| 300 kHz - 3 MHz
| 1 km - 100 m
| AM medium-wave broadcasts, amateur radio, avalanche beacons
|-
| High frequency
| HF
| 3 - 30 MHz
| 100 m - 10 m
| Shortwave broadcasts, citizens' band radio, amateur radio and over-the-horizon aviation communications, RFID, Over-the-horizon radar, Automatic link establishment (ALE) / Near Vertical Incidence Skywave (NVIS) radio communications, Marine and mobile radio telephony
|-
| Very high frequency
| VHF
| 30 - 300 MHz
| 10 - 1 m
| FM, television broadcasts and line-of-sight ground-to-aircraft and aircraft-to-aircraft communications. Land Mobile and Maritime Mobile communications, amateur radio, weather radio
|-
| Ultra high frequency
| UHF
| 300 MHz - 3 GHz
| 1 m - 100 mm
| Television broadcasts, microwave ovens, microwave devices/communications, mobile phones, wireless LAN, Bluetooth, ZigBee, GPS and two-way radios such as Land Mobile, FRS and GMRS radios, amateur radio
|-
| Super high frequency
| SHF
| 3 - 30 GHz
| 100 - 10 mm
| Microwave devices/communications, wireless LAN, most modern radars, communications satellites, satellite television broadcasting, DBS, amateur radio
|-
| Extremely high frequency
| EHF
| 30 - 300 GHz
| 10 - 1 mm
| High-frequency microwave radio relay, microwave remote sensing, amateur radio, directed-energy weapon, millimeter wave scanner
|-
| Terahertz or Tremendously high frequency
| THz or THF
| 300 GHz - 3 THz
| 1 - 0.1 mm
| Terahertz imaging, ultrafast molecular dynamics, condensed-matter physics, terahertz time-domain spectroscopy, terahertz computing/communications, sub-mm remote sensing, amateur radio
|}

Applied Planetary Radio Astronomy

2011-09-22T12:02:53Z

Gge002: Added The Radio Sky and How to Observe It - by Jeff Lashley

File:Ch13.pdf

2011-09-22T12:01:31Z

Gge002: The Radio Sky and How to Observe It - by Jeff Lashley Ch.13

The Radio Sky and How to Observe It - by Jeff Lashley
Ch.13

File:Ch12.pdf

2011-09-22T12:01:21Z

Gge002: The Radio Sky and How to Observe It - by Jeff Lashley Ch.12

The Radio Sky and How to Observe It - by Jeff Lashley
Ch.12

File:Ch11.pdf

2011-09-22T11:59:34Z

Gge002: The Radio Sky and How to Observe It - by Jeff Lashley Ch.11

The Radio Sky and How to Observe It - by Jeff Lashley
Ch.11

File:Ch10.pdf

2011-09-22T11:59:03Z

Gge002: The Radio Sky and How to Observe It - by Jeff Lashley Ch.10

The Radio Sky and How to Observe It - by Jeff Lashley
Ch.10