The “Rest” of AY201b (v.2013) 4/11 (Th): A: Magnetic Fields M1: MHD Shocks (Mocz); J: Cosmic Rays (Christian) after-class assignment: watch Bryan Gaensler’s colloquium on Cosmic Magnetism 4/16 (Tues): A: Expansion of HII Regions and SNRs H:Photon “Workflow ” M1: Cas A (Christian); M2: HII/PDR (Tripathi); M3: Milky Way Bubbles (Chen) 4/18 (Th): A: Discussion of Disks/Planet Formation M1: NH3 Spectrum; J: Disk SEDs (MacGregor) 4/23 (Tues): A: (Instabilities, continued, e.g. ; Ionization fronts, e.g. ...or guest lecture from Sean Andrews) M1: Clumpy GMCs (Miller): M2: Nebula Spectra (Portillo); M3: Zeeman (Woolsey) 4/25 (Th): A/guest: HI Tomography Experiments, IGM M1: Ly-alpha Forest (Ting); J: G-P Effect (Ting) 4/30 (Tues): A: Concluding Discussion M1: μwave Foregrounds (Karkare); M2: Multiphase ISM (Alexander); M3: ISM Landmarks (Macgregor); J: Galaxy Winds (Alexander) Problem Set 4, coming soon: Shocks, Disk, IGM...
Transcript
The ldquoRestrdquo of AY201b (v2013)411 (Th) A Magnetic FieldsM1 MHD Shocks (Mocz) J Cosmic Rays (Christian)after-class assignment watch Bryan Gaenslerrsquos colloquium on Cosmic Magnetism
416 (Tues) A Expansion of HII Regions and SNRs HPhoton ldquoWorkflowrdquoM1 Cas A (Christian) M2 HIIPDR (Tripathi) M3 Milky Way Bubbles (Chen)
418 (Th) A Discussion of DisksPlanet FormationM1 NH3 Spectrum J Disk SEDs (MacGregor)
423 (Tues) A (Instabilities continued eg Ionization fronts egor guest lecture from Sean Andrews)M1 Clumpy GMCs (Miller) M2 Nebula Spectra (Portillo) M3 Zeeman (Woolsey)
430 (Tues) A Concluding DiscussionM1 microwave Foregrounds (Karkare) M2 Multiphase ISM (Alexander) M3 ISM Landmarks (Macgregor) J Galaxy Winds (Alexander)
Problem Set 4 coming soon Shocks Disk IGM
AY201b 4bull11bull13
Magnetic Fields in the ISM
Draine references Zeeman 53
RMDM111-113B in Molecular Clouds 3210
Shocks with Magnetic Fields 36
Good intro to synchrotron polarimetry Sofue Fujimoto amp Wielebinski 1986Comprehensive Review of ldquoMagnetic Fields in Galaxiesrdquo Beck amp Wielebinski 2013
Magnets in the Sky
rsaquo Lodge (1900) Non-detection of radio waves from Sun ldquoThere were too many terrestrial sources of disturbance to make the experiment feasible I donrsquot know that it might not possibly be successful in some isolated country place but the arrangement must be highly sensitive in order to succeedrdquo
rsaquo Hale (1908) Zeeman splitting in sunspots ldquothe intensity of the field comes out 1000 gaussesrdquo
rsaquo Alfveacuten (1937) cosmic ray confinement implies ldquothe existence of a magnetic field in interstellar spacerdquo
rsaquo Fermi (1949) ldquothe main process of acceleration [of cosmic rays] is due to magnetic fields which occupy interstellar spaces hellip the magnetic hellip is of the order of 5x10-6 gauss while its intensity is probably greater in the heavier cloudsrdquo
rsaquo Cooper amp Price (1962) Detection of interstellar Faraday rotation against lobes of Cen A
Lodge (1911)
Parkes polarimetry of Centaurus A(Cooper amp Price 1962)Slide 3 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
From AG (1989) Harvard PhysicsPhD Thesis
Goodman et al 1989 Goodman et al 1990
OH Zeeman effect in emission in a Molecular Cloud
Background Starlight Polarimetryin Dark Clouds
(ldquoMagneticrdquo explanations of Larsonrsquos Laws +)
hot
cold
~neutral ~ionized
direction polarimetry of synchrotron
radiation
strength Faraday rotation
(RMDM)
strength Zeeman Effect
direction dust polarimetry
strength ~Chandrasekhar-Fermi
Measuring B in the ISM (IGM)
From AG (1989) Harvard PhysicsPhD Thesis
The Chandrasekhar-Fermi Method
B = σv
σθ
4πρNcorr
= numerical factor times velocity dispersionpolarization dispersion
~modeling field strength from polarization map messinessmessyweak field
orderedstrong field
Simulations oftenimply Ncorr~4 in ldquodark cloudsrdquo
Polarization Maps
Spectral-linemaps
Extinctiondust emissionor spectral-line
maps
Crutcher et al 2010
Modern View of Zeeman measurements of B in ISM
10 microG
1 mG
01 microG
100 cm-3 106 cm-3104 cm-3
no increase
~flux freez
ing
For reference(from Heiles et al 1990)
Cosmic Magnetism
rsaquo High-z seed fields B ~ 10-30 ndash10-20 G (Widrow 2002 Subramanian 2007)
rsaquo Intergalactic Medium B gt 10-15 G rsaquo Intracluster Medium B ~ 01-1 microG rsaquo Interstellar medium B ~ 1 microG ndash 10 mG rsaquo Galactic Center B ~ 50 microG ndash 1 mG
(Crocker et al 2010 Ferriegravere 2010) rsaquo Main sequence star HD 215441 B0 asymp 34 kG
(Babcock 1960) rsaquo White dwarf PG 1031+234 B0 asymp 109 G
(Schmidt et al 1986) rsaquo Pulsar PSR J1847-0130 B0 asymp 9 x 1013 G
(McLaughlin et al 2003) rsaquo Magnetar SGR 1806-20 B0 asymp 2 x 1015 G
(Kouveliotou et al 1998 Israel et al 2005) Bi asymp 1016 G rsaquo Cosmic strings (Ostriker et al 1986) B ~ 1030 G rsaquo Planck-mass monopoles B ~ 1055 G
(Duncan et al 2000)
Magnetic filam
ents in Perseus A
(Fabian et al 2008) G
alactic Center
(Yusef-Zadeh et al 1984) S
GR
1806-20 giant flare (N
AS
A)
Slide 4 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Do the Neutral amp Ionized Medium Have the Same B
Optical Polarimetry amp Comparison Scarrott 1987 Radio Data Fletcher et al 2011
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Superconductivity Lab Oslo University
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permissionmatching video at
1740-2400
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Pulsar B1154-62 (Gaensler et al 1998)
RM = +495 plusmn 6 rad m-2
matching video at
1740-2400
The Faraday Grid
Philipp Kronberg Physics TodaySlide 7 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
AY201b 4bull11bull13
Magnetic Fields in the ISM
Draine references Zeeman 53
RMDM111-113B in Molecular Clouds 3210
Shocks with Magnetic Fields 36
Good intro to synchrotron polarimetry Sofue Fujimoto amp Wielebinski 1986Comprehensive Review of ldquoMagnetic Fields in Galaxiesrdquo Beck amp Wielebinski 2013
Magnets in the Sky
rsaquo Lodge (1900) Non-detection of radio waves from Sun ldquoThere were too many terrestrial sources of disturbance to make the experiment feasible I donrsquot know that it might not possibly be successful in some isolated country place but the arrangement must be highly sensitive in order to succeedrdquo
rsaquo Hale (1908) Zeeman splitting in sunspots ldquothe intensity of the field comes out 1000 gaussesrdquo
rsaquo Alfveacuten (1937) cosmic ray confinement implies ldquothe existence of a magnetic field in interstellar spacerdquo
rsaquo Fermi (1949) ldquothe main process of acceleration [of cosmic rays] is due to magnetic fields which occupy interstellar spaces hellip the magnetic hellip is of the order of 5x10-6 gauss while its intensity is probably greater in the heavier cloudsrdquo
rsaquo Cooper amp Price (1962) Detection of interstellar Faraday rotation against lobes of Cen A
Lodge (1911)
Parkes polarimetry of Centaurus A(Cooper amp Price 1962)Slide 3 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
From AG (1989) Harvard PhysicsPhD Thesis
Goodman et al 1989 Goodman et al 1990
OH Zeeman effect in emission in a Molecular Cloud
Background Starlight Polarimetryin Dark Clouds
(ldquoMagneticrdquo explanations of Larsonrsquos Laws +)
hot
cold
~neutral ~ionized
direction polarimetry of synchrotron
radiation
strength Faraday rotation
(RMDM)
strength Zeeman Effect
direction dust polarimetry
strength ~Chandrasekhar-Fermi
Measuring B in the ISM (IGM)
From AG (1989) Harvard PhysicsPhD Thesis
The Chandrasekhar-Fermi Method
B = σv
σθ
4πρNcorr
= numerical factor times velocity dispersionpolarization dispersion
~modeling field strength from polarization map messinessmessyweak field
orderedstrong field
Simulations oftenimply Ncorr~4 in ldquodark cloudsrdquo
Polarization Maps
Spectral-linemaps
Extinctiondust emissionor spectral-line
maps
Crutcher et al 2010
Modern View of Zeeman measurements of B in ISM
10 microG
1 mG
01 microG
100 cm-3 106 cm-3104 cm-3
no increase
~flux freez
ing
For reference(from Heiles et al 1990)
Cosmic Magnetism
rsaquo High-z seed fields B ~ 10-30 ndash10-20 G (Widrow 2002 Subramanian 2007)
rsaquo Intergalactic Medium B gt 10-15 G rsaquo Intracluster Medium B ~ 01-1 microG rsaquo Interstellar medium B ~ 1 microG ndash 10 mG rsaquo Galactic Center B ~ 50 microG ndash 1 mG
(Crocker et al 2010 Ferriegravere 2010) rsaquo Main sequence star HD 215441 B0 asymp 34 kG
(Babcock 1960) rsaquo White dwarf PG 1031+234 B0 asymp 109 G
(Schmidt et al 1986) rsaquo Pulsar PSR J1847-0130 B0 asymp 9 x 1013 G
(McLaughlin et al 2003) rsaquo Magnetar SGR 1806-20 B0 asymp 2 x 1015 G
(Kouveliotou et al 1998 Israel et al 2005) Bi asymp 1016 G rsaquo Cosmic strings (Ostriker et al 1986) B ~ 1030 G rsaquo Planck-mass monopoles B ~ 1055 G
(Duncan et al 2000)
Magnetic filam
ents in Perseus A
(Fabian et al 2008) G
alactic Center
(Yusef-Zadeh et al 1984) S
GR
1806-20 giant flare (N
AS
A)
Slide 4 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Do the Neutral amp Ionized Medium Have the Same B
Optical Polarimetry amp Comparison Scarrott 1987 Radio Data Fletcher et al 2011
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Superconductivity Lab Oslo University
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permissionmatching video at
1740-2400
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Pulsar B1154-62 (Gaensler et al 1998)
RM = +495 plusmn 6 rad m-2
matching video at
1740-2400
The Faraday Grid
Philipp Kronberg Physics TodaySlide 7 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
Magnets in the Sky
rsaquo Lodge (1900) Non-detection of radio waves from Sun ldquoThere were too many terrestrial sources of disturbance to make the experiment feasible I donrsquot know that it might not possibly be successful in some isolated country place but the arrangement must be highly sensitive in order to succeedrdquo
rsaquo Hale (1908) Zeeman splitting in sunspots ldquothe intensity of the field comes out 1000 gaussesrdquo
rsaquo Alfveacuten (1937) cosmic ray confinement implies ldquothe existence of a magnetic field in interstellar spacerdquo
rsaquo Fermi (1949) ldquothe main process of acceleration [of cosmic rays] is due to magnetic fields which occupy interstellar spaces hellip the magnetic hellip is of the order of 5x10-6 gauss while its intensity is probably greater in the heavier cloudsrdquo
rsaquo Cooper amp Price (1962) Detection of interstellar Faraday rotation against lobes of Cen A
Lodge (1911)
Parkes polarimetry of Centaurus A(Cooper amp Price 1962)Slide 3 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
From AG (1989) Harvard PhysicsPhD Thesis
Goodman et al 1989 Goodman et al 1990
OH Zeeman effect in emission in a Molecular Cloud
Background Starlight Polarimetryin Dark Clouds
(ldquoMagneticrdquo explanations of Larsonrsquos Laws +)
hot
cold
~neutral ~ionized
direction polarimetry of synchrotron
radiation
strength Faraday rotation
(RMDM)
strength Zeeman Effect
direction dust polarimetry
strength ~Chandrasekhar-Fermi
Measuring B in the ISM (IGM)
From AG (1989) Harvard PhysicsPhD Thesis
The Chandrasekhar-Fermi Method
B = σv
σθ
4πρNcorr
= numerical factor times velocity dispersionpolarization dispersion
~modeling field strength from polarization map messinessmessyweak field
orderedstrong field
Simulations oftenimply Ncorr~4 in ldquodark cloudsrdquo
Polarization Maps
Spectral-linemaps
Extinctiondust emissionor spectral-line
maps
Crutcher et al 2010
Modern View of Zeeman measurements of B in ISM
10 microG
1 mG
01 microG
100 cm-3 106 cm-3104 cm-3
no increase
~flux freez
ing
For reference(from Heiles et al 1990)
Cosmic Magnetism
rsaquo High-z seed fields B ~ 10-30 ndash10-20 G (Widrow 2002 Subramanian 2007)
rsaquo Intergalactic Medium B gt 10-15 G rsaquo Intracluster Medium B ~ 01-1 microG rsaquo Interstellar medium B ~ 1 microG ndash 10 mG rsaquo Galactic Center B ~ 50 microG ndash 1 mG
(Crocker et al 2010 Ferriegravere 2010) rsaquo Main sequence star HD 215441 B0 asymp 34 kG
(Babcock 1960) rsaquo White dwarf PG 1031+234 B0 asymp 109 G
(Schmidt et al 1986) rsaquo Pulsar PSR J1847-0130 B0 asymp 9 x 1013 G
(McLaughlin et al 2003) rsaquo Magnetar SGR 1806-20 B0 asymp 2 x 1015 G
(Kouveliotou et al 1998 Israel et al 2005) Bi asymp 1016 G rsaquo Cosmic strings (Ostriker et al 1986) B ~ 1030 G rsaquo Planck-mass monopoles B ~ 1055 G
(Duncan et al 2000)
Magnetic filam
ents in Perseus A
(Fabian et al 2008) G
alactic Center
(Yusef-Zadeh et al 1984) S
GR
1806-20 giant flare (N
AS
A)
Slide 4 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Do the Neutral amp Ionized Medium Have the Same B
Optical Polarimetry amp Comparison Scarrott 1987 Radio Data Fletcher et al 2011
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Superconductivity Lab Oslo University
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permissionmatching video at
1740-2400
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Pulsar B1154-62 (Gaensler et al 1998)
RM = +495 plusmn 6 rad m-2
matching video at
1740-2400
The Faraday Grid
Philipp Kronberg Physics TodaySlide 7 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
From AG (1989) Harvard PhysicsPhD Thesis
Goodman et al 1989 Goodman et al 1990
OH Zeeman effect in emission in a Molecular Cloud
Background Starlight Polarimetryin Dark Clouds
(ldquoMagneticrdquo explanations of Larsonrsquos Laws +)
hot
cold
~neutral ~ionized
direction polarimetry of synchrotron
radiation
strength Faraday rotation
(RMDM)
strength Zeeman Effect
direction dust polarimetry
strength ~Chandrasekhar-Fermi
Measuring B in the ISM (IGM)
From AG (1989) Harvard PhysicsPhD Thesis
The Chandrasekhar-Fermi Method
B = σv
σθ
4πρNcorr
= numerical factor times velocity dispersionpolarization dispersion
~modeling field strength from polarization map messinessmessyweak field
orderedstrong field
Simulations oftenimply Ncorr~4 in ldquodark cloudsrdquo
Polarization Maps
Spectral-linemaps
Extinctiondust emissionor spectral-line
maps
Crutcher et al 2010
Modern View of Zeeman measurements of B in ISM
10 microG
1 mG
01 microG
100 cm-3 106 cm-3104 cm-3
no increase
~flux freez
ing
For reference(from Heiles et al 1990)
Cosmic Magnetism
rsaquo High-z seed fields B ~ 10-30 ndash10-20 G (Widrow 2002 Subramanian 2007)
rsaquo Intergalactic Medium B gt 10-15 G rsaquo Intracluster Medium B ~ 01-1 microG rsaquo Interstellar medium B ~ 1 microG ndash 10 mG rsaquo Galactic Center B ~ 50 microG ndash 1 mG
(Crocker et al 2010 Ferriegravere 2010) rsaquo Main sequence star HD 215441 B0 asymp 34 kG
(Babcock 1960) rsaquo White dwarf PG 1031+234 B0 asymp 109 G
(Schmidt et al 1986) rsaquo Pulsar PSR J1847-0130 B0 asymp 9 x 1013 G
(McLaughlin et al 2003) rsaquo Magnetar SGR 1806-20 B0 asymp 2 x 1015 G
(Kouveliotou et al 1998 Israel et al 2005) Bi asymp 1016 G rsaquo Cosmic strings (Ostriker et al 1986) B ~ 1030 G rsaquo Planck-mass monopoles B ~ 1055 G
(Duncan et al 2000)
Magnetic filam
ents in Perseus A
(Fabian et al 2008) G
alactic Center
(Yusef-Zadeh et al 1984) S
GR
1806-20 giant flare (N
AS
A)
Slide 4 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Do the Neutral amp Ionized Medium Have the Same B
Optical Polarimetry amp Comparison Scarrott 1987 Radio Data Fletcher et al 2011
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Superconductivity Lab Oslo University
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permissionmatching video at
1740-2400
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Pulsar B1154-62 (Gaensler et al 1998)
RM = +495 plusmn 6 rad m-2
matching video at
1740-2400
The Faraday Grid
Philipp Kronberg Physics TodaySlide 7 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
hot
cold
~neutral ~ionized
direction polarimetry of synchrotron
radiation
strength Faraday rotation
(RMDM)
strength Zeeman Effect
direction dust polarimetry
strength ~Chandrasekhar-Fermi
Measuring B in the ISM (IGM)
From AG (1989) Harvard PhysicsPhD Thesis
The Chandrasekhar-Fermi Method
B = σv
σθ
4πρNcorr
= numerical factor times velocity dispersionpolarization dispersion
~modeling field strength from polarization map messinessmessyweak field
orderedstrong field
Simulations oftenimply Ncorr~4 in ldquodark cloudsrdquo
Polarization Maps
Spectral-linemaps
Extinctiondust emissionor spectral-line
maps
Crutcher et al 2010
Modern View of Zeeman measurements of B in ISM
10 microG
1 mG
01 microG
100 cm-3 106 cm-3104 cm-3
no increase
~flux freez
ing
For reference(from Heiles et al 1990)
Cosmic Magnetism
rsaquo High-z seed fields B ~ 10-30 ndash10-20 G (Widrow 2002 Subramanian 2007)
rsaquo Intergalactic Medium B gt 10-15 G rsaquo Intracluster Medium B ~ 01-1 microG rsaquo Interstellar medium B ~ 1 microG ndash 10 mG rsaquo Galactic Center B ~ 50 microG ndash 1 mG
(Crocker et al 2010 Ferriegravere 2010) rsaquo Main sequence star HD 215441 B0 asymp 34 kG
(Babcock 1960) rsaquo White dwarf PG 1031+234 B0 asymp 109 G
(Schmidt et al 1986) rsaquo Pulsar PSR J1847-0130 B0 asymp 9 x 1013 G
(McLaughlin et al 2003) rsaquo Magnetar SGR 1806-20 B0 asymp 2 x 1015 G
(Kouveliotou et al 1998 Israel et al 2005) Bi asymp 1016 G rsaquo Cosmic strings (Ostriker et al 1986) B ~ 1030 G rsaquo Planck-mass monopoles B ~ 1055 G
(Duncan et al 2000)
Magnetic filam
ents in Perseus A
(Fabian et al 2008) G
alactic Center
(Yusef-Zadeh et al 1984) S
GR
1806-20 giant flare (N
AS
A)
Slide 4 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Do the Neutral amp Ionized Medium Have the Same B
Optical Polarimetry amp Comparison Scarrott 1987 Radio Data Fletcher et al 2011
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Superconductivity Lab Oslo University
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permissionmatching video at
1740-2400
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Pulsar B1154-62 (Gaensler et al 1998)
RM = +495 plusmn 6 rad m-2
matching video at
1740-2400
The Faraday Grid
Philipp Kronberg Physics TodaySlide 7 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
The Chandrasekhar-Fermi Method
B = σv
σθ
4πρNcorr
= numerical factor times velocity dispersionpolarization dispersion
~modeling field strength from polarization map messinessmessyweak field
orderedstrong field
Simulations oftenimply Ncorr~4 in ldquodark cloudsrdquo
Polarization Maps
Spectral-linemaps
Extinctiondust emissionor spectral-line
maps
Crutcher et al 2010
Modern View of Zeeman measurements of B in ISM
10 microG
1 mG
01 microG
100 cm-3 106 cm-3104 cm-3
no increase
~flux freez
ing
For reference(from Heiles et al 1990)
Cosmic Magnetism
rsaquo High-z seed fields B ~ 10-30 ndash10-20 G (Widrow 2002 Subramanian 2007)
rsaquo Intergalactic Medium B gt 10-15 G rsaquo Intracluster Medium B ~ 01-1 microG rsaquo Interstellar medium B ~ 1 microG ndash 10 mG rsaquo Galactic Center B ~ 50 microG ndash 1 mG
(Crocker et al 2010 Ferriegravere 2010) rsaquo Main sequence star HD 215441 B0 asymp 34 kG
(Babcock 1960) rsaquo White dwarf PG 1031+234 B0 asymp 109 G
(Schmidt et al 1986) rsaquo Pulsar PSR J1847-0130 B0 asymp 9 x 1013 G
(McLaughlin et al 2003) rsaquo Magnetar SGR 1806-20 B0 asymp 2 x 1015 G
(Kouveliotou et al 1998 Israel et al 2005) Bi asymp 1016 G rsaquo Cosmic strings (Ostriker et al 1986) B ~ 1030 G rsaquo Planck-mass monopoles B ~ 1055 G
(Duncan et al 2000)
Magnetic filam
ents in Perseus A
(Fabian et al 2008) G
alactic Center
(Yusef-Zadeh et al 1984) S
GR
1806-20 giant flare (N
AS
A)
Slide 4 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Do the Neutral amp Ionized Medium Have the Same B
Optical Polarimetry amp Comparison Scarrott 1987 Radio Data Fletcher et al 2011
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Superconductivity Lab Oslo University
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permissionmatching video at
1740-2400
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Pulsar B1154-62 (Gaensler et al 1998)
RM = +495 plusmn 6 rad m-2
matching video at
1740-2400
The Faraday Grid
Philipp Kronberg Physics TodaySlide 7 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
Crutcher et al 2010
Modern View of Zeeman measurements of B in ISM
10 microG
1 mG
01 microG
100 cm-3 106 cm-3104 cm-3
no increase
~flux freez
ing
For reference(from Heiles et al 1990)
Cosmic Magnetism
rsaquo High-z seed fields B ~ 10-30 ndash10-20 G (Widrow 2002 Subramanian 2007)
rsaquo Intergalactic Medium B gt 10-15 G rsaquo Intracluster Medium B ~ 01-1 microG rsaquo Interstellar medium B ~ 1 microG ndash 10 mG rsaquo Galactic Center B ~ 50 microG ndash 1 mG
(Crocker et al 2010 Ferriegravere 2010) rsaquo Main sequence star HD 215441 B0 asymp 34 kG
(Babcock 1960) rsaquo White dwarf PG 1031+234 B0 asymp 109 G
(Schmidt et al 1986) rsaquo Pulsar PSR J1847-0130 B0 asymp 9 x 1013 G
(McLaughlin et al 2003) rsaquo Magnetar SGR 1806-20 B0 asymp 2 x 1015 G
(Kouveliotou et al 1998 Israel et al 2005) Bi asymp 1016 G rsaquo Cosmic strings (Ostriker et al 1986) B ~ 1030 G rsaquo Planck-mass monopoles B ~ 1055 G
(Duncan et al 2000)
Magnetic filam
ents in Perseus A
(Fabian et al 2008) G
alactic Center
(Yusef-Zadeh et al 1984) S
GR
1806-20 giant flare (N
AS
A)
Slide 4 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Do the Neutral amp Ionized Medium Have the Same B
Optical Polarimetry amp Comparison Scarrott 1987 Radio Data Fletcher et al 2011
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Superconductivity Lab Oslo University
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permissionmatching video at
1740-2400
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Pulsar B1154-62 (Gaensler et al 1998)
RM = +495 plusmn 6 rad m-2
matching video at
1740-2400
The Faraday Grid
Philipp Kronberg Physics TodaySlide 7 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
Cosmic Magnetism
rsaquo High-z seed fields B ~ 10-30 ndash10-20 G (Widrow 2002 Subramanian 2007)
rsaquo Intergalactic Medium B gt 10-15 G rsaquo Intracluster Medium B ~ 01-1 microG rsaquo Interstellar medium B ~ 1 microG ndash 10 mG rsaquo Galactic Center B ~ 50 microG ndash 1 mG
(Crocker et al 2010 Ferriegravere 2010) rsaquo Main sequence star HD 215441 B0 asymp 34 kG
(Babcock 1960) rsaquo White dwarf PG 1031+234 B0 asymp 109 G
(Schmidt et al 1986) rsaquo Pulsar PSR J1847-0130 B0 asymp 9 x 1013 G
(McLaughlin et al 2003) rsaquo Magnetar SGR 1806-20 B0 asymp 2 x 1015 G
(Kouveliotou et al 1998 Israel et al 2005) Bi asymp 1016 G rsaquo Cosmic strings (Ostriker et al 1986) B ~ 1030 G rsaquo Planck-mass monopoles B ~ 1055 G
(Duncan et al 2000)
Magnetic filam
ents in Perseus A
(Fabian et al 2008) G
alactic Center
(Yusef-Zadeh et al 1984) S
GR
1806-20 giant flare (N
AS
A)
Slide 4 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Do the Neutral amp Ionized Medium Have the Same B
Optical Polarimetry amp Comparison Scarrott 1987 Radio Data Fletcher et al 2011
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Superconductivity Lab Oslo University
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permissionmatching video at
1740-2400
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Pulsar B1154-62 (Gaensler et al 1998)
RM = +495 plusmn 6 rad m-2
matching video at
1740-2400
The Faraday Grid
Philipp Kronberg Physics TodaySlide 7 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
Do the Neutral amp Ionized Medium Have the Same B
Optical Polarimetry amp Comparison Scarrott 1987 Radio Data Fletcher et al 2011
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Superconductivity Lab Oslo University
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permissionmatching video at
1740-2400
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Pulsar B1154-62 (Gaensler et al 1998)
RM = +495 plusmn 6 rad m-2
matching video at
1740-2400
The Faraday Grid
Philipp Kronberg Physics TodaySlide 7 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Superconductivity Lab Oslo University
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permissionmatching video at
1740-2400
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Pulsar B1154-62 (Gaensler et al 1998)
RM = +495 plusmn 6 rad m-2
matching video at
1740-2400
The Faraday Grid
Philipp Kronberg Physics TodaySlide 7 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
rsaquo Optical starlight polarizationrsaquo Synchrotron emission polarization B (orientation but not direction)rsaquo Infrared dust polarizationrsaquo Zeeman splitting B (long integrations high-density)
rsaquo Faraday rotation amp rotation measure (RM) are powerful probes of B
- radio wavelengths attenuation of radiation
- ldquoabsorptionrdquo experiment- provides direction of B- sensitive probe of ne
Mapping Magnetic Fields
RM asymp 220 rad mminus2 ne003 cm-3( ) B||
3 microG$
amp( L
3 kpc( )
Slide 6 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Pulsar B1154-62 (Gaensler et al 1998)
RM = +495 plusmn 6 rad m-2
matching video at
1740-2400
The Faraday Grid
Philipp Kronberg Physics TodaySlide 7 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
The Faraday Grid
Philipp Kronberg Physics TodaySlide 7 of Bryan Gaenslerrsquos 32113 ldquoCosmic Magnetismrdquo CfA Colloquium reproduced with permission
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
Excerpts from
ldquoMagnetic Fields in Galaxiesrdquo
Beck amp Wielebinski 2013
Note these maps are measures using intrinsic synchrotron polarization(not background sources)
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
Naiumlveteacute or the Simplest Analytic ModelsThe waywe once thoughtpolarization maps might lookhellip(c 1990)
(or)
Disk + Star
Core
Dark Cloud Theory 2
Dark Cloud Theory 1
A Truly Theoretical Set of Polarization Maps
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
Polarization Two Distances ldquoinrdquo Peseus
Goodman et al 1990
Mystery(Partially)Solved
see Ridge et al 2006
Rest of Solution3D Slicer Demo
Tilley amp Pudritz 2007
Early Magnetohydrodynamic Simulations
Strong Fieldβ=001 M=7
Weak Fieldβ=1 M=7
Synthetic Polarization Maps from Ostriker Stone amp Gammie 2001 see also Heitsch et al 2001 Padoan et al 2003
![Radio Time-Domain Signatures of Magnetar Birthsurveygizmoresponseuploads.s3.amazonaws.com/fileuploads/... · 2019-03-11 · magnetar remnants as well [52]. Indeed, there is evidence](https://static.documents.pub/doc/80x56/5f910083d47f1337ad0a63ef/radio-time-domain-signatures-of-magnetar-birthsurveygizmoresponseuploadss3-2019-03-11.jpg)
