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What’s Up for Imagers

What’s Up for Imagers. The Orion Region November 2008. Credit: Dave Kodama. Whazzup Here?. Huge molecular cloud in the Orion-Monoceros region A large swarm of very hot O and B stars – an “OB” association Numerous famous emission and reflection nebulae. Credit: John Gleason.

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What’s Up for Imagers

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  1. What’s Up for Imagers The Orion Region November 2008

  2. Credit: Dave Kodama

  3. Whazzup Here? • Huge molecular cloud in the Orion-Monoceros region • A large swarm of very hot O and B stars – an “OB” association • Numerous famous emission and reflection nebulae

  4. Credit: John Gleason

  5. Orion Molecular Cloud • The overall cloud contains something like 2x105 solar masses • Not just molecular hydrogen… • Spectroscopic signatures of nearly 150 molecules observed in these clouds • “Exotics” include benzene, acetic acid, and formaldehyde

  6. Orion Molecular Cloud • The portion within Orion is about ½ that, separated into ‘A’ and ‘B’ regions • Roughly associated with M42 and the Flame nebula, respectively • Areas of intense star formation • Eastern edge roughly marked by Barnard’s loop

  7. Credit: Rob Gendler

  8. Credit: J. Thibert, SSRO

  9. Credit: Steve Mazlin, SSRO

  10. Orion OB1 Association • OB Associations • Loose, co-moving stellar groups of Type O and early B-type stars • Typical lifetimes of < 30M years • Often found along the edge of a spiral arm as part of a density gradient • Internal age differences suggest successive “triggering” events

  11. Orion OB1 Association • Brightest stars in Orion are very young type O and B stars • 1a, 1b (Belt region), 10-12 million years old • 1c (Sword region), 3-6 million years old • 1d (Orion Nebula and Trapezium cluster), 1-4 million years old

  12. Credit: Rob Gendler

  13. Credit: HST

  14. Where Does M42 Fit In?

  15. Credit: HST

  16. The Trapezium C, Mag. 5.1 F, Mag. 10.2 A, Mag 6.7-7.5 D, Mag. 6.7 E, Mag. 10.3 B, Mag 8-8.5 The ‘F’ and ‘E’ components can be resolved with amateur scopes The Trapezium is “in front of” the huge molecular cloud Magnitudes

  17. Credit: HST

  18. Credit: HST

  19. Protoplanetary Disks • Rotating disk of dense gas around a new star • Flattened because of rotation in the collapsing gas • Initial collapse takes about 105 years; ongoing accretion for about 107 years • Often “shredded” by radiation from bright stars – this creates the “coma” shape

  20. Computer-simulated proto-planetary disk, San Diego Super-computer Center

  21. Credit: J. C. Casado, APOD 12/1/97

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