radio astronomy emission mechanisms. nrao/aui/nsf3 omega nebula
TRANSCRIPT
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Radio Astronomy Radio Astronomy Emission Emission
MechanismsMechanisms
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NRAO/AUI/NSF 4
Recipe for Radio WavesRecipe for Radio Waves
Thermal Continuum RadiationThermal Continuum Radiation(Black Body Radiation)(Black Body Radiation)
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NRAO/AUI/NSF 5
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NRAO/AUI/NSF 6
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NRAO/AUI/NSF 7
Thermal or Black Body Emission
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Thermal Continuum Radiation
• Characteristics:
– Opaque “Black” Body
– Isothermal
– In Equilibrium
• Planck’s Law:
– I = Intrinsic Intensity (ergs/cm2/sec/Hz).
– h = Planck’s Constant
– k = Boltzman’s Constant
– T in K
– ν in Hz
• Radio Approximation:
Ih c
ehkT
3 2
1
IkT
c
2 2
2
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NRAO/AUI/NSF 9
Recipe for Radio WavesRecipe for Radio Waves
Non-Thermal Continuum RadiationNon-Thermal Continuum RadiationWhenever a charge particle is acceleratedWhenever a charge particle is accelerated
1.1.Free-Free EmissionFree-Free Emission
•Hot (5000 K) Ionized GasesHot (5000 K) Ionized Gases• Planetary NebulaePlanetary Nebulae• HII RegionsHII Regions
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NRAO/AUI/NSF 10
Electron accelerates as it passes near a proton.
Electromagnetic waves are released
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Planetary Nebula and HII Regions
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NRAO/AUI/NSF 12
Free free emission
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NRAO/AUI/NSF 13
Non-Thermal Continuum RadiationNon-Thermal Continuum Radiation
Whenever a charge particle is accelerated Whenever a charge particle is accelerated
1.1.Free-Free EmissionFree-Free Emission
2.2.Synchrotron RadiationSynchrotron Radiation
• Strong magnetic fieldStrong magnetic field
• Ionized gases moving at relativistic velocitiesIonized gases moving at relativistic velocities
Recipe for Radio WavesRecipe for Radio Waves
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NRAO/AUI/NSF 14
Electrons accelerate around magnetic field lines
Electromagnetic waves are released
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NRAO/AUI/NSF 15
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NRAO/AUI/NSF 17
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NRAO/AUI/NSF 18
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NRAO/AUI/NSF 20
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NRAO/AUI/NSF 21
Spectral Line RadiationAtomic and molecular transitionsAtomic and molecular transitions
Recipe for Radio WavesRecipe for Radio Waves
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NRAO/AUI/NSF 22
Gas SpectraNeon
Sodium
Hydrogen
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Spectral-Line RadiationRecombination Lines
• Ionized regions (HII regions and planetary nebulae)
• Free electrons temporarily recaptured by a proton
• Atomic transitions between outer orbital (e.g., N=177 to M = 176)
3 3 1 01 11 5
2 2.m n
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Hyperfine Transition of Hydrogen
• Found in regions where H is atomic (HI).
• Spin-flip transition
– Electron & protons have “spin”
– In a H atoms, spins of proton andelectron may be aligned or anti-aligned.
– Aligned state has more energy.
– Difference in Energy = h * frequency
• Frequency = 1420.4058 MHz
– An aligned H atom will take 11 million years to flip
– But, 1067 atoms in Milky Way
• 1052 H atoms per second emit at 1420 MHz.
NRAO/AUI/NSF 24
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NRAO/AUI/NSF 25
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NRAO/AUI/NSF 26
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NRAO/AUI/NSF 27
Doppler Shift
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NRAO/AUI/NSF 28
Doppler Shift
• c = speed of light = 3 x 105 km/sec
• Rest Frequency = 1420.4058 MHz for the hyperfine transition of Hydrogen
• If V > 0, object is moving away from us
• If V < 0, object is moving toward us.
ystFrequencRe
equencyObservedFrystFrequencRecVelecity
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Spectral-Line RadiationMilky Way Rotation and Mass?
• For any cloud
– Observed velocity = difference between projected Sun’s motion and projected cloud motion.
• For cloud B
– The highest observed velocity along the line of site
– VRotation = Vobserved + Vsun*sin(L)
– R = RSun * sin(L)
• Repeat for a different angle L and cloud B
– Determine VRotation(R)
– From Newton’s law, derive M(R) from V(R)
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Missing Mass
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Interstellar Molecules• About 90% of the over 140 interstellar molecules discovered with
radio telescopes.
• Rotational (electric dipole) Transitions
• Up to thirteen atoms
• Many carbon-based (organic)
• Many cannot exist in normal laboratories (e.g., OH)
• H2 most common molecule:
– No dipole moment so no radio transition.
– Only observable in UV (rotational) or Infrared (vibrational) transitions.
– Astronomers use CO as a tracer for H2
• A few molecules (OH, H2O, …) maser
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Molecules Discovered by the GBT
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Discovery of Ethanol
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Interstellar Molecule Formation
• Need high densities (100 –106 H atoms/cm3)
– Lots of dust needed to protect molecules for stellar UV• Form in dust clouds = Molecular Clouds• Associated with stars formation
– But, optically obscured – need radio telescopes
• Low temperatures (< 100 K)
• Some molecules (e.g., H2) form on dust grains
• Most form via ion-molecular gas-phase reactions
– Exothermic
– Charge transfer
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Grain Chemistry
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Ion-molecular gas-phase reactionsExamples of types of reactions
C+ + H2 → CH2+ + hν (Radiative Association)
H2+ + H2 → H3
+ + H (Dissociative Charge Transfer)H3
+ + CO → HCO+ + H2 (Proton Transfer)H3
+ + Mg → Mg+ + H2 + H (Charge Transfer)He+ + CO → He + C+ + O (Dissociative Charge Transfer)HCO+ + e → CO + H (Dissociative)C+ + e → C + hν (Radiative)Fe+ + grain → Fe + hν (Grain)
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NRAO/AUI/NSF 43
Organic Organic Molecules;Molecules;
Seeds of LifeSeeds of Life
Organic Organic Molecules;Molecules;
Seeds of LifeSeeds of Life
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