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X-Ray Properties of Orion's Young Massive Stars

X-Ray Properties of Orion's Young Massive Stars. Norbert S. Schulz Paola Testa David P. Huenemoerder Claude R. Canizares Arik Mitschang Joy Nichols. The HETG Orion Legacy Project. Advisory: J. H. Kastner, D. Weintraub, S. Shukla, F. Favata, F. Reale, M. Gagne, N. Walborn, T. Preibisch.

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X-Ray Properties of Orion's Young Massive Stars

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  1. X-Ray Properties of Orion's Young Massive Stars Norbert S. Schulz Paola Testa David P. Huenemoerder Claude R. Canizares Arik Mitschang Joy Nichols The HETG Orion Legacy Project Advisory: J. H. Kastner, D. Weintraub, S. Shukla, F. Favata, F. Reale, M. Gagne, N. Walborn, T. Preibisch Great Barriers, Townsville QL, Sep. 13 2010

  2. X-ray Properties of Massive Stars X-Ray Properties of Orion's Young Massive Stars Standard Model vs Colliding Winds Massive Star-forming Regions The Orion Trapezium HETG Orion Legacy Project Update Magnetic Properties of Trapezium Stars Great Barriers, Townsville QL, Sep. 13 2010

  3. (Exotic) X-ray Production in Hot Stars • Radiation Driven Stellar Wind: • - momentum through line absorption • - momentum - luminosity relation • - soft X-rays from wind shocks • - opacity effects • Colliding Wind Plasmas: • - very early type binaries / WR binaries • - WR 140 , h Carina • Magnetically Confined Wind: • - same as above but: • - existence of strong global B field • - mass loss vs. B field strength • - hard X-rays from dense hot • plasma disk near Alfven radius • Magnetically Confined Local Plasma: • - hot emission line stars • Binary Induced Magnetic Reconnection Great Barriers, Townsville QL, Sep. 13 2010

  4. Soft X-rays from wind shocks The X-ray prototype of O stars: z Pup (Cassinelli et al. 2001, Kahn et al. 2001) Great Barriers, Townsville QL, Sep. 13 2010

  5. Hard X-rays from colliding winds The enigmatic system Eta Carina:: (Corcoran et al. 2003, Corcoran 2006) Great Barriers, Townsville QL, Sep. 13 2010

  6. Townsley et al. 2003 – 2006 Brandt et al. 2006 Massive Star-forming Regions:30 Doradus and M17 Great Barriers, Townsville QL, Sep. 13 2010

  7. Massive Star-forming Regions:The Very Large Carina Project Great Barriers, Townsville QL, Sep. 13 2010

  8. Massive Star-forming Regions:The Orion Nebula Cluster Great Barriers, Townsville QL, Sep. 13 2010

  9. Feigelson et al. 2005 COUP Schulz et al. 2002 ACIS-S/HETG Massive Star-forming Regions:The Orion Nebula Cluster Great Barriers, Townsville QL, Sep. 13 2010

  10. Massive Star-forming Regions:The Orion Trapezium Cluster Great Barriers, Townsville QL, Sep. 13 2010

  11. Massive Stars in the Orion Trapezium Q1 Ori B1: B1V B2: B3V (Petr et al. 1998) Q1 Ori A: B0V (O9.7V), likely triple (ref) • Q1 Ori C1: O5.5Vp (34 Msun) • C2: O9.5 (15.5 Msun) • (Kraus et a. 2007) Q1 Ori D1: B0V D2: B5/K0 (Kraus et al 2007) Q2 Ori A: O9.5V, close 3 - 7 Msun companion (0.43 AU) , dist. < 9 Msun companion (173 AU) (Abt et al. 1991, Preibisch et al. 1999) Great Barriers, Townsville QL, Sep. 13 2010

  12. The HETG Orion Legacy Project • Scope: • Obtain high quality X-ray spectra of • - the massive Trapezium stars (> 3 Msun) • - > a dozen class II/III spectra of T Tauri stars • - giant flares • Science: • - Accretion in PMS stars • - Coronal activity in YSOs • - Magnetically Confined Winds • - Colliding Winds • - Fe fluoresence • Exposure: 1 week (586 ks) Great Barriers, Townsville QL, Sep. 13 2010

  13. Star type log Lx [erg/s] M [Msun] T [MK] coronal Q1 Ori B1 B1V 30.2 10 5 -- 10 no Massive Star-forming Regions:The Orion Trapezium Cluster Q1 Ori B2 B3V < 29 8 N/A no Q1 Ori D1 B0V 29.8 16 2 -- 7 no Q1 Ori C1 O5.5V 33.1 35.5 7 -- 84 MCWM Q1 Ori A1 B0V 31.6 15.5 12 -- 55 MCWM ? Q2Ori A1 O9.5V 31.6 25.5 2 -- 25 MCWM Q1 Ori E GIII/GIII 32.7 3.5/3.5 12 -- 75 coronal Great Barriers, Townsville QL, Sep. 13 2010

  14. Star type log Lx [erg/s] M [Msun] T [MK] coronal Q1 Ori B1 B1V 30.2 10 5 -- 10 no Massive Star-forming Regions:The Orion Trapezium Cluster Q1 Ori B2 B3V < 29 8 N/A no Q1 Ori D1 B0V 29.8 16 2 -- 7 no Q1 Ori C1 O5.5V 33.1 35.5 7 -- 84 MCWM Q1 Ori A1 B0V 31.6 15.5 12 -- 55 MCWM ? Q2Ori A1 O9.5V 31.6 25.5 2 -- 25 MCWM Q1 Ori E GIII/GIII 32.7 3.5/3.5 12 -- 75 coronal Great Barriers, Townsville QL, Sep. 13 2010

  15. Extreme X-Ray Sources in Orion: Q2Ori A: Outbursts • Lines are symmetric • Temperatures: 10 – 65 MK • Lines are unresolved < 50 km s-1 • Rion >> 2 Rstar (Ralven) • ===> Standard Coronal Plasma Properties Great Barriers, Townsville QL, Sep. 13 2010

  16. Comparison with evolved Hot Stars Emission Measure: Line Widths: Coronal Coronal Coronal MCW? MCW MCW MCW Q2 Ori A Great Barriers, Townsville QL, Sep. 13 2010 (Wojdowski & Schulz 2005)

  17. Young (< 1 M yr) central O5 binary (DeRose et al. 2009, Wolk et al. 2003) Massive Star-forming Regions:Next nearest; RCW38 Great Barriers, Townsville QL, Sep. 13 2010

  18. Conclusions • Massive Trapezium stars show a variety of unusual phenomena • Q1 Ori B,C,D show that young massive ZAMS are X-ray weak unless they are enhanced by external interactions (see also Trifid [Rho et al. 2003]) • X-Ray enhancement in Orion is most likely all due to magnetic interactions, i.e. in form of magnetic wind confinement and some forms of coronal (mag. reconnection events) emissions • No evidence for colliding winds Questions & (Greater) Barriers: • Why is Orion’s massive core so different with respect to other massive cluster cores? • Why appear Orion’s massive stars magnetic while massive stars in other clusters do not? • Where are the colliding wind binaries? • Why are Q1 Ori A and D so fundamentally different in X-rays? • Could Q1 Ori E provide a coronal link to the X-ray production in HAEBE stars Great Barriers, Townsville QL, Sep. 13 2010

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