GALILEO MEETING Nobeyama 10/11 July, 2002 UK BCS PRESENTATION Len Culhane Mullard Space Science Laboratory University College London

SUMMARY Brief history of BCS concept Summary of instrument properties Some scientific highlights People involved in Galileo project Proposed contribution from BCS team

Original BCS Prototype Flown on NASA Aerobee Sounding Rockets First results from the prototype published in: "A New Type of Crystal Spectrometer for Solar X-ray Studies", J.L. Culhane, R.C. Catura, E.G. Joki, J.C. Bakke and C.G. Rapley, 1974, Mon. Not. R. astr. Soc., 168, 217. Prototype used a curved KAP crystal and operated in the range 8 – 17Å. It obtained solar active region spectra with several strong Fe lines. Demonstration of BCS operation led to its selection as part of the X-ray Polychromator instrument, with L.W. Acton as PI, on NASA’s Solar Maximum Mission

Mounting of the BCS in Yohkoh

Plasma Upflow Velocities for Flare of 16 December, 1991 (Culhane, Inda, et al., 1994, Solar Physics) Velocities are determined from two component fits to the Ca XIX resonance line profile High velocity flow is initiated following energy deposition by non-thermal electron impact in the Chromosphere. Hard X-ray burst light curve profiles the electron beam impact. Plasma upflow occurs during and just after the hard X-ray burst but the upflow velocity returns to the AR value after the peak of the Ca XIX light curve

Evolution of Ca XIX Resonance Line Profile for the Flare of

Evaporation and the Slope of the Accelerated Electron Spectrum (McDonald, Culhane, Harra, 1999, Sol. Phys.) 16th December, nd February, 1992 _____ Total Energy Evap. Energy  = 4.0  = 3.0 Accelerated electron spectrum: dN/dE = kE -  Steep spectrum leads to enhanced evaporation

V nt = [2k (T LW - T e )/M] 0.5 = 0 for T LW = T e Line Broadening and Non-thermal Velocity For a limb flare there can be no line of sight velocity components. Excess width (T LW >T e ) above the thermal Doppler value could be due to turbulence in upflowing plasma or directly related to energy release. (Khan et al., Ap. J., 1995) Yohkoh BCS Ca XIX impulsive phase spectrum is illustrated.

SXT HXT Flare A BCS S XV Spectrum Flare B SXT HXT HXT and BCS S XV Light Curves Pre-flare Development of V nt in AR 7590 on 3 Oct., 1993 (Harra, Matthews, Culhane, 2001, Ap. J. Lett.)

Flare A Flare B V nt HXT V nt and HXT (15 – 25 keV) plotted against time for two Flares on 3 Oct., 1993 (Harra et al., 2001) V nt falls after flare A to a minimum of 40 km/s at 09:13 UT. This value is characteristic of active region plasma. It then rises steadily over 11 min. to reach ~ 100 km/s at 09:25 UT - the start of hard X-ray emission by flare B. There is evidence for pre-flare B magnetic flux emergence in AR 7590

Coronal Plasma Parameter Scaling with Photospheric Magnetic Field (van Driel-Gesztelyi et al. ) Tests of Heating Models (Demoulin et al.) The evolution of AR 7978 has been studied over five rotations from birth to decay Only AR 7978 was present, so BCS was used to measure plasma parameters as was SXT. Spectra show T e evolution MDI measured total magnetic flux for emergence and six CMPs Observations show AR and AR = a B av b. Values of b were established for,, and that are consistent for BCS and SXT. Models allowed by the range of exponents favour magnetic field stressing models rather than those based on wave heating

People Involved MSSLNRL -Bentley- Brown -Culhane- Doschek -Foley- Mariska - Harra RALNAOJ - Lang- Watanabe

Summary of Proposed BCS Contribution - I BCS data in agreed FITS Format Input to Legacy book: –Full instrument description –Updated instrument guide –Report on instrument calibration –Spectral fitting routines with comments –Summary of discoveries with major BCS role –BCS contribution to a mission-wide bibliography

Summary of Proposed BCS Contribution - II BCS spectra – photon units vs wavelength BCS SXV and Ca XIX time spectrograms – one per orbit BCS flare catalogue that matches GOES event list above a “tbd” threshold In flight cal data – approx 10 calibration data sets through the mission

Wavelength Time Spectrogram – approach I

Spectrogram – approach II

Interaction with UK SURF and European Grid of Solar Observatories (EGSO) The Solar UK Research Facility (SURF) is the new name for Yohkoh Data Archive Centre (YDAC) UK BCS Galileo activities will be organized within SURF There is also a UK ASTROGRID project with solar data involvement – SURF will maintain contact with ASTROGRID Galileo FITS headers should ideally be compatible with EGSO catalogues EGSO FITS headers should contain certain key words The EGSO project is at an early stage and seeks a continued dialog with Galileo - RDB is interacting with the Galileo FITS working group Continuing dialog is sought in particular on data provision, access and related security issues A draft FITS header document has been distributed to the attendees at this meeting

END OF PRESENTATION

Flare A Flare B BCS S XV Spectrum HXT SXT HXT SXT Pre-flare Development of V nt in AR 7590 on 3 Oct., 1993 (Harra, Matthews, Culhane, 2001, Ap. J. Lett.) HXT and BCS S XV Light Curves