radio astronomy emission mechanisms. nrao/aui/nsf3 omega nebula

Radio Astronomy Radio Astronomy Emission Emission

MechanismsMechanisms

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Recipe for Radio WavesRecipe for Radio Waves

Thermal Continuum RadiationThermal Continuum Radiation(Black Body Radiation)(Black Body Radiation)

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Thermal or Black Body Emission

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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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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Electron accelerates as it passes near a proton.

Electromagnetic waves are released

Planetary Nebula and HII Regions

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Free free emission

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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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Electrons accelerate around magnetic field lines

Electromagnetic waves are released

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Spectral Line RadiationAtomic and molecular transitionsAtomic and molecular transitions

Recipe for Radio WavesRecipe for Radio Waves

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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

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.

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Doppler Shift

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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

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

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

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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Organic Organic Molecules;Molecules;

Seeds of LifeSeeds of Life

Organic Organic Molecules;Molecules;

Seeds of LifeSeeds of Life