I have been studying EVE H. S. Hudson Space Sciences Laboratory, University of California, Berkeley, USA Astronomy & Astrophysics Group, Glasgow Berkeley.

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Presentation transcript:

I have been studying EVE H. S. Hudson Space Sciences Laboratory, University of California, Berkeley, USA Astronomy & Astrophysics Group, Glasgow Berkeley Jan. 26, 2011

Motivation: global spectrum Berkeley Jan. 26, 2011 Hudson et al THz WLF EUV

More motivation Berkeley Jan. 26, 2011 Milligan & Dennis 2009

Still more motivation Berkeley Jan. 26, 2011 Kowalski et al. 2010

…and yet more motivation Berkeley Jan. 26, 2011 Peter et al.1990

Flare SOL T00:57 Berkeley Jan. 26, 2011 Martinez-Oliveros et al. 2011

Flare SOL T00:57 Berkeley Jan. 26, 2011 Martinez-Oliveros et al Eve 304A

Sun-as-a-star EUV tools SOHO/SEM: broad EUV band at nm SDO/EVE MEGS-A: far-UV, 1 A resolution, 10 s cadence (data available) SDO/EVE MEGS-B: near-UV, 1 A resolution, 10 s cadence (to be released in a week or so) SDO/EVE ESP (broad EUV bands, 0.25 s cadence) Berkeley Jan. 26, 2011

Line detail, total and subtracted Berkeley Jan. 26, 2011 Flare vs preflare Impulsive vs gradual

Doppler shift? Berkeley Jan. 26, 2011

EVE 304A for SOL T00:57 Berkeley Jan. 26, 2011

Calibration nm => /30.4 c or about 6 km/s Berkeley Jan. 26, 2011

Calibration nm => /30.4 c or about 6 km/s Amazing! Berkeley Jan. 26, 2011

304 time series, one day Berkeley Jan. 26, 2011

Flux and Doppler, one day Berkeley Jan. 26, 2011

EVE 304 narrow vs SEM Berkeley Jan. 26, 2011

EVE 304 vs SEM, broad Berkeley Jan. 26, 2011

EVE 304, SEM, EVE broad Berkeley Jan. 26, 2011

Broad passband Berkeley Jan. 26, 2011

Comments on EVE Lots of lines to work with He II spectrum in the impulsive phase (can see Ly-  and a hint of Ly-  in SOL ) Need bigger flares Looking forward to near UV (out to 1500A, I think) as a part of WLF characterization Berkeley Jan. 26, 2011

EVE ESP and SOL Berkeley Jan. 26, 2011

ESP 304A for SOL Berkeley Jan. 26, 2011

EVE 304 narrow vs SEM Berkeley Jan. 26, 2011

Conclusions The SDO data for the Sun “as a star” are rather fine There are many applications of these data - Global flare spectra - Doppler shifts / flare dynamics - Charge-exchange components - Seismology (classical) - Seismology (coronal) Berkeley Jan. 26, 2011