2010
DOI: 10.1051/0004-6361/201014587
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Star formation triggered by H II regions in our Galaxy

Abstract: Context. It has been shown that by means of different physical mechanisms the expansion of H ii regions can trigger the formation of new stars of all masses. This process may be important to the formation of massive stars but has never been quantified in the Galaxy. Aims. We use Herschel-PACS and -SPIRE images from the Herschel infrared survey of the Galactic plane, Hi-GAL, to perform this study. Methods. We combine the Spitzer-GLIMPSE and -MIPSGAL, radio-continuum and submillimeter surveys such as ATLASGAL wi… Show more

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Cited by 80 publications
(78 citation statements)
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“…However, advancing ionization fronts and expanding superbubbles can also compress nearby clouds and thereby trigger the formation of new generations of stars (e.g., Reach et al 2004;Cannon et al 2005;Oey et al 2005;Preibisch & Zinnecker 2007;Deharveng et al 2009;Zavagno et al 2010;Brand et al 2011). The interaction of the massive stars with the surrounding clouds and the balance between cloud destruction and triggered star formation determine the characteristics and the final outcome of the star formation process (see Dale et al 2007;Dale & Bonnell 2008;Bate 2009;Gritschneder et al 2010, for numerical studies).…”
Section: Introductionmentioning
confidence: 99%
“…However, advancing ionization fronts and expanding superbubbles can also compress nearby clouds and thereby trigger the formation of new generations of stars (e.g., Reach et al 2004;Cannon et al 2005;Oey et al 2005;Preibisch & Zinnecker 2007;Deharveng et al 2009;Zavagno et al 2010;Brand et al 2011). The interaction of the massive stars with the surrounding clouds and the balance between cloud destruction and triggered star formation determine the characteristics and the final outcome of the star formation process (see Dale et al 2007;Dale & Bonnell 2008;Bate 2009;Gritschneder et al 2010, for numerical studies).…”
Section: Introductionmentioning
confidence: 99%
“…The stellar content of these condensations is described in detail in Zavagno et al (2007) and in Deharveng et al (2009). The properties of the point sources observed in this region with Herschel PACS and SPIRE are described in Zavagno et al (2010a). An off position (OFF) was obtained to serve as a reference.…”
Section: Pointingsmentioning
confidence: 99%
“…This region contains a massive Class 0 source revealed with Herschel (Zavagno et al 2010a) and a chain of young, lower mass stars ). -C2: this condensation contains a bright Class I source and is, as C1, also located on the southern (and densest) border of the PDR.…”
Section: Pointingsmentioning
confidence: 99%
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“…A few individual bubbles have been studied well, such as N22 (Ji et al 2012), N49 (Watson et al 2008;Deharveng et al 2010;Zavagno et al 2010), N65 (Petriella et al 2010), N68 (Zhang & Wang 2012b), and S51 (Zhang & Wang 2012a). There are many models and observations to explain the dusty windblown bubbles, such as bubble N49 of Everett & Churchwell (2010).…”
Section: Introductionmentioning
confidence: 99%