Charge Exchange in Comets off the beaten track
description
Transcript of Charge Exchange in Comets off the beaten track
Dennis Bodewits1,
Damian Christian2, Casey Lisse3, Scott Wolk4, Konrad Dennerl5, Jenny Carter6, Andy Read6,
and Susan Lepri7
(1) Univ. Maryland, College Park, (2) CSU Northridge, (3) JHU/APL, (4) CfA, (5) MPE Garching, Germany, (6) Univ. Leicester, UK, (7) Univ. Michigan
Charge Exchange in Cometsoff the beaten track
AAS/HEAD 2013
Outline
• Charge Exchange occurs where a hot plasma meets a neutral gas.
• How can we use other wavelength regimes?• How can we use comets to study CX emission
in different plasma environments?• What will we learn with the next generation X-
ray telescopes?
A High Energy View of Comets
X-rayOptical
Dust (Continuum)
MoleculesNH2, C3, C2, NH, OH, CS, H2
Molecular ionsCO+, H2O+, CO2+, ..
Energy Wavelength
AtomsS, C, O, H
UV FUV EUV
IonsHe+, He2+, O6+, ..
Heavy IonsC5,6+, O7,8+, ..
Comet
Solar Wind
Simultaneous X-ray/UV image of a comet
APOD Feb 21, 2009, Bodewits et al. 2010, Carter et al. 2011
1. Other X-rays
Chandra Comet SurveyC,N OVII OVIII
A
B
C
D
E
G
F
H
X-ray spectra sample solar wind statelow abundance of highly charged oxygen cold windhigh abundance of highly charged oxygen hot wind
Bodewits et al. 2007
Sola
r win
d fr
eeze
-in Te
mpe
ratu
re
Temperature vs. Freeze-in Temperature
Bodewits et al. 2012
Bodewits et al. 2007
Where is the Polar wind?
OVII and OVIIINe X
Ne IX Mg XI
Mg XIISi XIII
Bodewits et al. 2007; Ewing et al. 2013.
Fe XV - XX
Comet emission > 1000 eVC/2002 C1 (Ikeya-Zhang) + CME
Si
Mg
SWCX or artifact?
Mg XI, XII?
Si XIII, XIV?
• 73P/Schwassmann-Wachmann 3b• 0.1 AU in 2006• Warm slow wind
ACE Chandra
C6+/O7+ 2.1 ± 0.7 2.1 ± 1.0
C5+/O7+ 7.6 ± 3 87 ± 29
• Cross section?• Calibration around 300 eV?• CX emission from Mg, Si, Ne…
• 90% of emission at 300 eV is NOT CV
SWCX <300 eV: terra incognita
SWCX <300 eV: terra incognita
Sasseen et al. 2006
CHIPS+Chandra observations of Comet C/2001 Q4 (NEAT)
Koutroumpa et al. 2008
SWCX Model
Si
Mg
Si and Mg as temperature probes
2. The UltraViolet: Helium Rules!
OVI: elusive SWCX emission• N(O6+) = ~10 – 20 x N(O7+)• OVI doublet around 103 nm• Doppler-shift measure SW velocity• Emission cross section comparable to
OVII features (Bodewits & Hoekstra 2007). Increase 2-3x with velocity.
• Fuse: non-detections in 3 comets (Weaver et al. 2002; Feldman et al. 2005).
• 400x smaller FOV than CXO• Best target: high inclination comet in
polar wind• Rosetta ALICE
103.1, 103.7 nm
Most abundant ions in SW emit in EUV: O6+ + H2O O5+(nl)
Bodewits & Hoekstra 2007
fast
slow
OVI Line Ratio 11.6 / 17.0 nm
• 1 – 10% of SW• N(He) ~ 75 xN(O)• Cross sections 1/10th
• Fully ionized
• Giotto (Fuselier ‘91)
• EUVE– He I 58.4 nm Hale-Bopp
(Krasnopolsky et al. ‘97)– He II 30.4 nm Hyakutake (Krasnopolsky
et al. ‘01)
– Venus, Mars (Krasnopolsky & Gladstone ’05)
He2+
He+
He
30.4 nm
58.4 nm
He: The Coolest Ion of Them All
He II/He I Line RatioHe He+
Electron capture strongly depends on collision partner and velocity
Bodewits et al (2004, 2006)
3. The Next Generation
Existing Observations:XMM & Suzaku Archives
SUZAKU - 73P
Brown et al. 2010 Dennerl et al. In prep.
XMM RGS – C/2000 WM1
Prospects of High Resolution Spectroscopy
•High resolution X-ray spectroscopy will reveal: features of minor species (Fe, Mg, Si)
•will allow direct measurements of the triplet/singlet ratios of CV and OVII
•may detect fluorescence features of molecules such as CO2 (Dennerl et al. 2006)
•may find continuum emission (5% of total – Krasnopolsky et al. 1997)
•Should have capabilities below 300 eV•Imaging would be awesome! (not discussed here)
Wide Field Imager at GSFC?
C/2012 S1 (ISON)The Great Comet of 2013?
Seiic
hi Y
oshi
da
Swift – Bodewits et al. 2013
Thank You!