Observational signatures of self- consistent 3D CME-flare ... · consistent 3D CME-flare models...
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Observational signatures of self-consistent 3D CME-flare models
J.J. Drake1, O. Cohen2, J.D. Alvarado-Gomez1 and C. Garraffo1
1Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge
2Lowell Center for Space Science and Technology, 600 Suffolk Street, Lowell
S.P. Moschou1,
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NASA
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NASA
SDO
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Drake et al, 2013
NASA
SDO
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Drake et al, 2013
What have we learned from the Sun?
NASA
SDO
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The CME-flare scenario
Shibata et al., ApJ, 1995
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Benz, 2002
Summary of observations
Kontar et al., PRL, 2017
SDO/AIA 193 Å
HXR SXR UV
Radio
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Acceleration processes
• RECONNECTION: ‣ High efficiency ‣ Collisionless & fast ‣ Multiple magnetic islands => merge => accelerate e- => HXR
Desai & Burgess, JGR, 2008
Reconnection .vs. Shocks • Both met from solar and stellar
flares to AGN jets (Sironi+,2015) and supernovae shock waves.
• SHOCKS: ~ 10% efficiency (Lin 2011)
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What don’t we know yet?• CMEs and flares (& particle
acceleration) different manifestations of a single grand process or not?
• Acceleration mechanisms ‣ Acceleration onset e- ‣ Relative importance
• Exactly how do e- escape the flaring site not understood at all
Desai & Burgess, JGR, 2008
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What don’t we know yet?• CMEs and flares (& particle
acceleration) different manifestations of a single grand process or not?
• Acceleration mechanisms ‣ Acceleration onset e- ‣ Relative importance
• Exactly how do e- escape the flaring site not understood at all
Desai & Burgess, JGR, 2008
Simulations
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3D MHD-EPIC simulationsGlobal MHD (BATS-R-US) + local implicit Particle-in-Cell (iPIC3D )
Hall MHD vs MHD-EPIC, Daldorff et al., JCP, 2014
2D
Hall MHD vs MHD-EPIC, Toth et al., JGR, 2016
3D
Successful Magnetospheric Studies
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MHD region
Solar Corona
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MHD region
Solar Corona
Reconnection site
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MHD region
Solar Corona
iPIC3D region
Reconnection site
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MHD region
Solar Corona
Thermal X-Rays
Hard X-Rays
Non-thermal e-
acceleratediPIC3D region
Reconnection site
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Daldorff et al., JCP, 2014
Two-way coupling
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Simulations to Lynx • Acceleration onset and efficiency • Thermal—non-thermal component • Heating-cooling in time • Synthetic views in different wavelengths • Emission profiles in up to strong stellar B • CME-flare relation
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What about stellar flares?• Flaring activity depends on B, which depends on the
stellar characteristics. • Many X-ray stellar flares (1st Reise+,ApJ,1975) • X-ray flares F–M stars indicating energetic transient
events (~min-hours) & magnetic reconnection (e.g. Güdel & Nazé 2009).
• Large stellar flares T~100 MK (e.g. Osten+2005, 2007), while solar peak T~20–30 MK.
• Evidence of HXR persisting throughout the entire flare time evolution (Osten et al. 2007)
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Stellar flares
Güdel et al. 2002 XMM-Newton
• Large flare on Proxima Centauri (Güdel et al. 2002, 2004) Chromospheric evaporation evidence, n < 1010 => 4x1011 cm-3
• Neupert Effect (1968): LU(t) ∝ dLX(t)/dt (e.g. Güdel+2002)
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Stellar flares
Güdel et al. 2002 XMM-Newton
• Large flare on Proxima Centauri (Güdel et al. 2002, 2004) Chromospheric evaporation evidence, n < 1010 => 4x1011 cm-3
• Neupert Effect (1968): LU(t) ∝ dLX(t)/dt (e.g. Güdel+2002)
Lynx: will improve quality spectra with time slices resolving fast processes
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Summary of observations What could Lynx observe?
Hara et al., Apj, 2011
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Summary of observations What could Lynx observe?
Hara et al., Apj, 2011
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Summary of observations What could Lynx observe?
Hara et al., Apj, 2011
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Summary of observations What could Lynx observe?
Hara et al., Apj, 2011
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Summary of observations What could Lynx observe?
Hara et al., Apj, 2011
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Summary of observations What could Lynx observe?
Hara et al., Apj, 2011
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Summary of observations What could Lynx observe?
Hara et al., Apj, 2011R=10,000=>v~30km/s
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Conclusions and summary• Sun valuable laboratory, but ‣ Does not provide all the answers
• Stellar flares might drastically change the picture • Lynx observations hopefully will shed light into: ‣ Densities, temperatures, emitting volumes and masses
of hot plasma in stellar flares ‣ May help disentangle thermal—non-thermal
components ‣ Resolve fast processes ‣ Provide insights on acceleration processes ‣ Blueshift measurements of relevant flows, maybe
even chromospheric evaporation?