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Star formation activity in cores wit...

Chambers, Edward T.

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Star formation activity in cores within infrared dark clouds.

紀錄類型:	書目-語言資料,印刷品 : Monograph/item
正題名/作者:	Star formation activity in cores within infrared dark clouds./
作者:	Chambers, Edward T.
面頁冊數:	184 p.
附註:	Source: Dissertation Abstracts International, Volume: 70-10, Section: B, page: 6270.
Contained By:	Dissertation Abstracts International70-10B.
標題:	Physics, Astronomy and Astrophysics. -
電子資源:	http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=3382561
ISBN:	9781109436006

Star formation activity in cores within infrared dark clouds.
Chambers, Edward T.

Star formation activity in cores within infrared dark clouds. - 184 p.

Source: Dissertation Abstracts International, Volume: 70-10, Section: B, page: 6270.

Thesis (Ph.D.)--Boston University, 2010.

In this dissertation, I probe the star formation activity of cores within infrared dark clouds (IRDCs). IRDCs are identified as extinction features against the bright Galactic plane at infrared wavelengths. They are dense, cold, and massive, conditions expected for clouds that host the elusive earliest stages of high-mass star formation. A sample of 38 IRDCs was mapped in 1.2 mm continuum emission using the Institut de Radioastronomie Millimetrique (IRAM) 30m Telescope. These data show that each IRDC contains at least one compact, dense core, and most IRDCs contain several cores. This dissertation focuses on a sample of 190 cores found within these 38 IRDCs.

ISBN: 9781109436006Subjects--Topical Terms:

1019521
Physics, Astronomy and Astrophysics.

Star formation activity in cores within infrared dark clouds.
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245 1 0 $a Star formation activity in cores within infrared dark clouds.
300 $a 184 p.
500 $a Source: Dissertation Abstracts International, Volume: 70-10, Section: B, page: 6270.
500 $a Adviser: James M. Jackson.
502 $a Thesis (Ph.D.)--Boston University, 2010.
520 $a In this dissertation, I probe the star formation activity of cores within infrared dark clouds (IRDCs). IRDCs are identified as extinction features against the bright Galactic plane at infrared wavelengths. They are dense, cold, and massive, conditions expected for clouds that host the elusive earliest stages of high-mass star formation. A sample of 38 IRDCs was mapped in 1.2 mm continuum emission using the Institut de Radioastronomie Millimetrique (IRAM) 30m Telescope. These data show that each IRDC contains at least one compact, dense core, and most IRDCs contain several cores. This dissertation focuses on a sample of 190 cores found within these 38 IRDCs.
520 $a Some cores within IRDCs display several indicators of star formation. Among these signatures are extended, enhanced 4.5 mum emission, which I call 'green fuzzies,' and 24 mum point sources. I have identified green fuzzies within the sample of 190 IRDC cores and subsequently correlated the green fuzzies with 24 mum point sources. I call cores within IRDCs that contain a green fuzzy coincident with a 24 mum point source 'active,' and I call cores within IRDCs that contain neither star formation indicator 'quiescent.' I also find additional cores that are dominated by 8 mum emission, which I call 'red.' I hypothesize that quiescent, active, and red cores form a star-forming evolutionary sequence within IRDCs.
520 $a I test this evolutionary sequence by comparing the sizes, densities, maser activity, and temperatures of the sample of 190 cores. I find that active cores are smaller and denser than quiescent cores, as expected if quiescent cores collapse to form active cores. I find that active and red cores are more likely to contain H2O and CH3OH masers (well-known signposts for star formation) than quiescent cores. Finally, I find that red cores are warmer than active cores, and that active cores are warmer than quiescent cores. Together, these results support the hypothesis that quiescent, active, and red cores form a star-forming evolutionary sequence within IRDCs.
590 $a School code: 0017.
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710 2 $a Boston University. $3 1017454
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790 1 0 $a Jackson, James M., $e advisor
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791 $a Ph.D.
792 $a 2010
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