Jeff Morgenthaler, Ph.D. Planetary Science Institute · 2013. 3. 26. · F b l id b i t t For...
Transcript of Jeff Morgenthaler, Ph.D. Planetary Science Institute · 2013. 3. 26. · F b l id b i t t For...
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Jeff Morgenthaler, Ph.D.Planetary Science Institute
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How to verify a lot of quantum h i l l l ti ith t d i mechanical calculations without doing
any quantum mechanics
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High-quality astrophysics with h l l h isophomore-level physics
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What I did for my summer vacation l t last year
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Mike Combi (U. Michigan)( g )Walt Harris (U.C. Davis)Paul Feldman (Johns Hopkins)(J p )Hal Weaver (Johns Hopkins Applied Physics Lab)Galaxy Evolution Explorer (GALEX) team
Karl Forster (Cal Tech)Tim Conrow (IPAC)Tim Conrow (IPAC)Susan Neff (NASA/GSFC)
JPL HORIZONS: Jon GiorginiJ O ONS: Jo G o g
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BackgroundBackgroundWhat is a comet – why do we care?How do we “measure” comets?Why do we need accurate molecular/atomic physics to measure comets?
h b l fMeasuring the carbon ionization lifetimeNext step: COAlong the way: OFinal phase: OH
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NC
Nucleus (10—100 km)Head/Coma (neutral
NA
SA/JPL
Caltech/U
M
emission lines, 100—106
km) – ballistic motionDust tail (white 107 km)
L-MD
/McR
Dust tail (white, 107 km)Ion tail (blue , 107 km)
Co
RhEL
opyright ©hem
ann(A ©
1997 by A
ustria) G
erald
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Comets are some of the most primordial material left over from the formation of the material left over from the formation of the solar system
Solar system formation modelsSolar system formation models
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Comets may have Comets may have delivered water and the seeds of life to Earth, maybe Mars, Venus, etc.
d h bAmino acids have been observed
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IDEAL: Cryogenic IDEAL: Cryogenic Nucleus Sample Return (CNSR)Bring back a core sampleBillions of d lldollarsNot any time
soon
Prialnik 2004
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Next best thing:Next best thing:Take the lab to the cometRosetta: European Space Agency (ESA) p g y ( )Orbiter/LanderComet 67P/Churyumov-Gerasimenko
Astrium - E. Viktor
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First approximation: First approximation: Stardust mission flew through the tail of comet Wild 2 collected comet dust
d t it b k t and sent it back to Earth
NASA
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Second approximation: Deep Impact impactorSecond approximation: Deep Impact impactorExcavated comet material
NA
MA
SA/JPL-C
Maryland/Co Caltech/U
nornell
niversity of
Deep Impact pre-impact view Stardust revisit
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Tried and true: Remote sensingg
Look at what is coming off of the comet and figure out what it is made ofVolatiles:Molecule 1P/HalleyH2O 100CO 3.5—11CO2 3—4CH4 <0.8C H 0 3
The Mayall 4-meter telescope at the KittPeak National Observatory near Tucson, Arizona.
C2H2 0.3C2H6 0.4CH3OH 1.8
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A i h h d iA spectrum is worth a thousand pictures103PP/H
artly22 (EPO
XI ttarget; Weeaver et al.. 1992)
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S i i Spectro-imaging is priceless
Carbon 1561 Å and 1657 Å and 1657 Å multiplets
Carbon comaCarbon coma
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NASA Small Explorer missionWorks for comets too!Works for comets too!
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Morrissey et al. 2005FUV
NUV UV
Weaver et al. 1992Weaver et al. 1992
FUV NUVVisible
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Different emission Different emission lines have differentscale lengthsg
NUV
S h d d t bSmushed data cube
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Mcphaate
et al. 19999
FUV NUV
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P d i Production rate, Q(C), derived from total from total emission
Q(C) related to C ( )in the nucleus
Reality: most i instruments don’t “swallow” all swallow all the light
Aperture pcorrections
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Require accurate knowledge of spatial distributionNow measured for carbon (Morgenthaler et al. 2011)
K Key parameters:τ = lifetimev = outflow
velocityvτ = scale length
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Haser (1957) model: Consider comet nucleus isotropicallyemitting particles at rate Q, velocity v, lifetime τ.D i ti i l ft i t th d ☺
τvr
e−
=Qn(r)
Derivation is left as an exercise to the reader ☺
2-component Haser model:π
evr 24
n(r)
n = number densityQ d i
2 component Haser model:“Parent/mother” = 1“Daughter” = 2k bi ti f l l thQ = production rate
τ = lifetimev = velocity
⎟⎟⎞
⎜⎜⎛
−=−−
22112
Qn(r) ττ vr
vr
eek
k = combination of scale lengths
yr = dist. from comet ⎟
⎠⎜⎝2
24n(r)
πeek
vr
Integrate along line of sight to convert number density to column density
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Carbon is a daughter speciesCarbon is a daughter speciesv1~ 1 km/s (bulk outflow velocity)v ~ 4 km/s (ejection velocity)v2~ 4 km/s (ejection velocity)> 3 x 105 km, just carbon ionization
Best-fit Haserd l d t i model determines
carbon ionization lifetime
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Best-fit Haser model determines carbon ionization Best-fit Haser model determines carbon ionization lifetime
Qk r−
22
224
Qk n(r) τ
πve
vr
−
=
Problem: BACKGROUND!
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Comet moves: Stars can be erasedComet moves: Stars can be erasedBackground exposure ~1 month prior – good enough?
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What changes over a FOV of 1 degree?What changes over a FOV of 1 degree?Not the GalaxyS l t ? FUV di l li ht t b i ht Solar system? FUV zodiacal light not bright enoughEarth’s atmosphere: AirglowEarth s atmosphere: Airglow
Photochemical effect
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C i i Correction is analogous to extinction
shadowextinctionSpent summer vacation
sun orbit
vacation picturing GALEX orbit and Earth’s shadow in 3DAeronomyy
Sujatha et al. (2009) airglow used solar activity
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Airglow ~uniform over 1 degreeConstant offset of background imageg g
Solar photoionization only
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Comet Machholz’s heliographic latitude was 30° during solar min Edge of slow solar wind zone
Morgenthaler et al. 2011
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F b l i d b i t t For carbon, solar wind can be more important than solar photoionization!IMPORTANT: standard reference (Huebner IMPORTANT: standard reference (Huebner, Keady, and Lyon 1992) only includes photoratesSolar wind ionization important for all long-lived species
Ph t lif ti > 500 000 Photo lifetimes > 500,000 se.g. H, C, O, CO
Previous production rates need to be revisited! Previous production rates need to be revisited! Comet “carbon puzzle” (Festou 1984) may be solved
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Verified ionization cross section calculations Verified ionization cross section calculations for carbon over a wide range of photon energies
Verified carbon-proton charge exchange cross p g gsection
Verified carbon-electron collisional cross section
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Verified ionization cross section calculations Verified ionization cross section calculations for carbon over a wide range of photon energies
Assume solar spectrum is well knownVerified carbon-proton charge exchange cross section
Assume solar wind speed and density well knownVerified carbon-electron collisional cross section
A d t i l l i dAssumed comet was in slow solar wind
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Mcphaate
et al. 19999
FUV NUV
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Next step:CO withCO withFUV grism
Morgenthaler et al. 2011
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Why does [OI] Why does [OI] oxygen distribution in Hale-Bopp look like a comet?Metastable [OI] prompt emission really traces H O really traces H2O and OH
Morgenthaler et al. 2001
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Residuals aren’t as cleanResiduals aren t as cleanNeed 3D coma models – jets, emission asymmetries ion lines?asymmetries, ion lines?
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It is possible to reliably measure atomic and It is possible to reliably measure atomic and molecular lifetimes using wide-field observations of comets
C was easy – isotropicCO will be harder with grism dataOH requires sophisticated coma models
GALEX could be used as an upper-atmosphere h t ti (700 k ltit d )research station (700 km altitude)