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High Energy Activity on Young Stellar Objects - Activity of the X-ray Lab. in 2005 -

High Energy Activity on Young Stellar Objects - Activity of the X-ray Lab. in 2005 -. Kenji Hamaguchi, Rob Petre. Activity of the X-ray Lab. Study of the X-ray activity on YSOs Intermediate-mass eclipsing binary, TY CrA X-ray monitoring of an FU/EX Ori outburst

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High Energy Activity on Young Stellar Objects - Activity of the X-ray Lab. in 2005 -

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  1. High Energy Activity on Young Stellar Objects- Activity of the X-ray Lab. in 2005 - Kenji Hamaguchi, Rob Petre

  2. Activity of the X-ray Lab. • Study of the X-ray activity on YSOs • Intermediate-mass eclipsing binary, TY CrA • X-ray monitoring of an FU/EX Ori outburst • X-ray activity on Herbig Ae/Be stars • New observations • Suzaku: 73P/Schwassmann-Wachmann 3 • XMM-Newton: a young eclipsing binary • Chandra & HST: HAes (collaboration w/C. Grady) • More Chandra proposal on this cycle (w/Carol)

  3. Outburst of V1647 Ori Strong correlation between optical/IR and X-rays X-ray emission is originated in mass accretion

  4. Activity of the X-ray Lab. • Study of the X-ray activity on YSOs • Intermediate-mass eclipsing binary, TY CrA • X-ray monitoring of an FU/EX Ori outburst • X-ray activity on Herbig Ae/Be stars • New observations • Suzaku: 73P/Schwassmann-Wachmann 3 • XMM-Newton: a young eclipsing binary • Chandra & HST: HAes (collaboration w/C. Grady) • More Chandra proposal on this cycle (w/Carol)

  5. Setbacks of Our Projects • ADP proposal for the archival research of the XMM data of star forming regions • ADP proposal was canceled last year. • Suzaku observations • The launch was delayed (July 2005). • It could not observe Tempel 9 at the Deep Impact. • The XRS detector malfunctioned before actual observations.

  6. Loss of XRS on Suzaku • XRS (X-ray calorimeter) • had the best energy resolution (E/dE ~1000) • malfunctioned before observations • Suzaku has two types of detectors working • XIS (X-ray CCD) and HXD • The spatial resolution is limited. • XIS BI chip has the best energy resolution so far below 1 keV for diffuse sources.

  7. Activity of the X-ray Lab. • Study of the X-ray activity on YSOs • Intermediate-mass eclipsing binary, TY CrA • X-ray monitoring of an FU/EX Ori outburst • X-ray activity on Herbig Ae/Be stars • New observations • Suzaku: 73P/Schwassmann-Wachmann 3 • XMM-Newton: a young eclipsing binary • Chandra & HST: HAes (collaboration w/C. Grady) • More Chandra proposal on this cycle (w/Carol)

  8. HD100453 (Chandra) EK Cep (XMM-Newton) New Data Have Just Arrived!

  9. Activity of the X-ray Lab. • Study of the X-ray activity on YSOs • Intermediate-mass eclipsing binary, TY CrA • X-ray monitoring of an FU/EX Ori outburst • X-ray activity on Herbig Ae/Be stars • New observations • Suzaku: 73P/Schwassmann-Wachmann 3 • XMM-Newton: a young eclipsing binary • Chandra & HST: HAes (collaboration w/C. Grady) • More Chandra proposal on this cycle (w/Carol)

  10. 10’ R CrA star forming region XMM-Newton, 2003 March 28 Red: 0.2-1 keV Green: 1-2 keV Blue: 2-9 keV

  11. TY CrA - the only eclipsing Herbig Be binary system confirmed - Fourth ~M4 0.3” (~40 AU) Primary B7-9 3.16Msolar 1-1.5 AU Tertiary 1.2~1.4Msolar 0.065 AU Orbital Period, 2.88878 days Secondary 1.64Msolar • X-ray observations • (ASCA: 1994-98) • kT ~ 1.5 keV • Lx ~ 3e30 ergs s-1 Age ~3 Myr

  12. TY CrA - the only eclipsing Herbig Be binary system confirmed - XMM-Newton Large effective area Best for observing time variation Secondary eclipse March 29, 2003 33ksec Primary eclipse March 28, 2003, 37ksec Orbital Period, 2.88878 days

  13. Simulations of X-ray light curves during the eclipse

  14. Secondary Eclipse

  15. Primary Eclipse

  16. X-ray Spectrum in the Primary Eclipse Primary eclipse kThot ~4 keV Log Lx ~ 2e31 (ergs s-1) Secondary eclipse kThot ~1.5 keV Log Lx ~ 6e30 (ergs s-1)

  17. Light Curve, Apr 2001 Secondary eclipse kThot ~4.5 keV Log Lx ~ 3e31 (ergs s-1) 0.4 0.49 Orbital Phase

  18. Summary of the Observations • Low State (XMM 2nd obs. & ASCA obs.) • kThot~1.5 keV, Lx ~3-6x1030 ergs s-1 • No variation specific at optical eclipses • Normal activity of some stars in the TY CrA system? • High State • kThot~4 keV, Lx ~2-3x1031ergs s-1 • X-ray flux increased at coincident with eclipsing phases (of both the primary and secondary) • Enhanced inter-binary magnetic activity? The X-ray beaming effect?

  19. X-ray Observations of TY CrA

  20. Diagram of the HAe X-ray Activity

  21. The high state originates from a temporal activity

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