SMESE: a French/ChineseSolar “SMEX”

H.S. Hudson

Space Sciences Lab, UC Berkeley

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Lyman- for the first time: the strongest transition of the most abundant element in the brightest object in the sky!

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DESIR - far IR instrument

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QuickTime™ and aMicrosoft Video 1 decompressorare needed to see this picture.

Xu et al. 2006

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HEBS - will they make the usual design mistakes?

Flare footpoints and ribbons:The impulsive phase

H.S. Hudson

Space Sciences Lab, UC Berkeley

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Contents

• History & Nomenclature

- Impulsive phase and gradual phase

- Other things (Krucker)• Magnetic changes (Fletcher)• TSI observations• Flares and CMEs (Zhang, Temmer)• Flare waves (Regnier?)• Implosions (Ji)• Conclusions

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Flare-related ionospheric effects

• SPA (“Sudden Phase Anomaly”) => soft X-rays• SFD (“Sudden Frequency Deviation”) => EUV burst• SCNA, SES, SWF, …

The Neupert effect could be anticipated in 1971 (or earlier) via the SPA/SFD comparison (Donnelly 1969)

Kane & Donnelly (1971) introduced the term “impulsive phase” (cf. Joan Vorpahl thesis; H “flash phase”)

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Kane & Donnelly 1971

Oda and Takakura observingsolar microwaves in 1948

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GONG

SOHO/MDI

B dB

Sudol & Harvey (2005), flare of 2003 Oct. 29,line-of-sight field differences

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Flare of 2001 Aug. 25:GONG + GOES

Other examples withGOES times

The changes are stepwise, of order10% of the line-of-sight field, andprimarily occur at the impulsive phase of the flare

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First detection of solar flarevia total irradiance: gradualand impulsive phases!

(Woods et al. 2004, 2006)

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CME acceleration at the impulsive phase

Zarro et al. 1999

Temmer 2008 (RHESSI ScienceNugget #71) http://sprg.ssl.berkeley.edu/~tohban/nuggets/

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Flare-related large-scale waves

• Metric type II wave / Moreton wave (blast wave)• Ejection-driven wave (CME bow shock)

- Mewaldt et al. (2004), Emslie et al. (2005) find

of order 10% total flare energy in SEPs

• Seismic wave in solar interior (Kosovichev-Zharkova)

• The motions of these waves originate in the field restructuring that provides the energy

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Implosive motion

Veronig et al. 2005

Hudson 2000

Liu et al. 2005

http://solarmuri.ssl.berkeley.edu/~hhudson/cartoons/

“Magnetoisobar”

“Bald patch”

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Conclusions

• The impulsive phase is extremely energetic• It can be seen all across the electromagnetic

spectrum and in mechanical forms as well• The impulsive phase is characterized by large-scale

effects reflecting intermittent and unresolved elements

• So… what is the physics of the impulsive phase?

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QuickTime™ and aTIFF (Uncompressed) decompressor

are needed to see this picture.

Fletcher & Hudson 2008

New description of the impulsive phase

http://solarmuri.ssl.berkeley.edu/~hhudson/cartoons/

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How does this cartoon help?• It is a useful application to astrophysics of lessons

learned in space plasmas • It takes a different and healthy approach to the major

flare problem of electron beam stability• It acknowledges a recent solar observational

breakthrough - the stepwise changes in BLOS observed in the photosphere below a flare

• It suggests the need for further stereoscopic observation after STEREO, e.g. Solar Orbiter and the Sentinels