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What Can We Learn About the Ejecta from Solar-B/EIS

What Can We Learn About the Ejecta from Solar-B/EIS. P. F. Chen 1,2 , D. H. Brooks 1 , H. Isobe 1 , K. Shibata 1. １． Kwasan Observatory, Kyoto University, Japan 2. Department of Astronomy, Nanjing University( 南京大学 ), China. From Our Simulations. Chen & Shibata, 2000, ApJ, 545, 524.

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What Can We Learn About the Ejecta from Solar-B/EIS

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  1. What Can We Learn About the Ejecta from Solar-B/EIS P. F. Chen1,2, D. H. Brooks1, H. Isobe1, K. Shibata1 １．Kwasan Observatory, Kyoto University, Japan 2. Department of Astronomy, Nanjing University(南京大学),China

  2. From Our Simulations Chen & Shibata, 2000, ApJ, 545, 524 Chen, Wu, Shibata, & Fang 2002, ApJ, 572, L99

  3. From the PIs • Scientific Objectives • Flare & CME onset process • Reconnection evidence • …… • Candidate Lines Ca XVII, Fe X--XV, Fe XXIII, Fe XXIV, Si VII, Si X

  4. VDEM & Forward Modeling • VDEM(Velocity differential Emission Measure) It is directly related to the flaring plasma properties • Why Forward Modeling • Inversion Modeling is an ill-posed problem, and should be combined with the Forward Modeling ( resolution of SOHO/CDS is not high enough) • To suggest the most suitable lines for the corresponding phenomenon Coronal Reconnection outflow & Moreton waves

  5. Scenario

  6. T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta Observer Ca XVII slit I Units I 3510-11 photons s-1 cmdetector-2 cmflare-2Å-1 VDEM 1015 photons s-1 (km s-1)-1 cmflare-2

  7. T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta Fe X Observer slit I Units I 3510-11 photons s-1 cmdetector-2 cmflare-2Å-1 VDEM 1015 photons s-1 (km s-1)-1 cmflare-2

  8. T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta Fe XI Observer slit I Units I 3510-11 photons s-1 cmdetector-2 cmflare-2Å-1 VDEM 1015 photons s-1 (km s-1)-1 cmflare-2

  9. T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta Fe XII Observer slit I Units I 3510-11 photons s-1 cmdetector-2 cmflare-2Å-1 VDEM 1015 photons s-1 (km s-1)-1 cmflare-2

  10. T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta Fe XIII Observer slit I Units I 3510-11 photons s-1 cmdetector-2 cmflare-2Å-1 VDEM 1015 photons s-1 (km s-1)-1 cmflare-2

  11. T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta Fe XIV Observer slit I Units I 3510-11 photons s-1 cmdetector-2 cmflare-2Å-1 VDEM 1015 photons s-1 (km s-1)-1 cmflare-2

  12. T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta Observer Fe XV slit I Units I 3510-11 photons s-1 cmdetector-2 cmflare-2Å-1 VDEM 1015 photons s-1 (km s-1)-1 cmflare-2

  13. T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta Fe XXIII Observer slit I Units I 3510-11 photons s-1 cmdetector-2 cmflare-2Å-1 VDEM 1015 photons s-1 (km s-1)-1 cmflare-2

  14. T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta Fe XXIV Observer slit I Units I 3510-11 photons s-1 cmdetector-2 cmflare-2Å-1 VDEM 1015 photons s-1 (km s-1)-1 cmflare-2

  15. T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta Si VII Observer slit I Units I 3510-11 photons s-1 cmdetector-2 cmflare-2Å-1 VDEM 1015 photons s-1 (km s-1)-1 cmflare-2

  16. T0=1.5 MK, n0=109 cm-3 Tmax =30 MK for flare loop top, & 12 MK for the ejecta Si X Observer Observer Observer slit slit slit I I I Units I 3510-11 photons s-1 cmdetector-2 cmflare-2Å-1 VDEM 1015 photons s-1 (km s-1)-1 cmflare-2

  17. Ｓｕｍｍａｒｙ Across the reconnection point upwardly • Ca XVII 192.8 Red shift blue shift with a possible 2 peaks at the blue wing corresponding to the slow shock pair • Fe X 190.04 Besides a static component, one red peak turns to 1-2 blue peaks • Fe XV 284.2 strong line, besides a static component, 1 2 1 blue peaks • Si X 258.4 strong line, besides a static component, 1-2 peaks at the blue wing from the erupting flux rope and CME expansion

  18. Future Research • Contamination from other lines • Jets at multiwavelengths • To construct a G function which weakly depends on T, a1G1+a2G2+a3G3+a4G4+a5G5+……

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