Triggered star formation in bright-rimmed clouds: the Eagle nebula revisited

Miao, Jingqi; White, G. J.; Nelson, Richard P.; Thompson, M. A.; Morgan, L. K.

doi:10.1111/j.1365-2966.2006.10260.x

Cited by 90 publications

(121 citation statements)

References 35 publications

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“…Another scenario for triggered star formation is contraction of a pre-existing clump due to radiation-driven implosion (Lefloch & Lazareff 1994;Kessel-Deynet & Burkert 2003;Miao et al 2006) or to a shock wave from the expanding H II region (Boss 1995). This scenario predicts a random distribution of molecular clumps around the H II region.…”

Section: A Scenario For Star Formation In the S233 Regionmentioning

confidence: 99%

Star formation in the S233 region

Ladeyschikov¹,

Соболев²,

Parfenov³

et al. 2015

Mon. Not. R. Astron. Soc.

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The main objective of this paper is to study the possibility of triggered star formation on the border of the H II region S233, which is formed by a B-star. Using high-resolution spectra we determine the spectral class of the ionizing star as B0.5 V and the radial velocity of the star to be −17.5 ± 1.4 km s −1 . This value is consistent with the velocity of gas in a wide field across the S233 region, suggesting that the ionizing star was formed from a parent cloud belonging to the S233 region. By studying spatial-kinematic structure of the molecular cloud in the S233 region, we detected an isolated clump of gas producing CO emission red-shifted relative to the parent cloud. In the UKIDSS and WISE images, the clump of gas coincides with the infrared source containing a compact object and bright-rimmed structure. The bright-rimmed structure is perpendicular to the direction of the ionizing star. The compact source coincides in position with IRAS source 05351+3549. All these features indicate a possibility of triggering formation of a next-generation star in the S233 region. Within the framework of a theoretical one-dimensional model we conclude that the 'collect-and-collapse' process is not likely to take place in the S233 region. The presence of the bright-rimmed structure and the compact infrared source suggest that the 'collapse of the pre-existing clump' process is taking place.

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Section: A Scenario For Star Formation In the S233 Regionmentioning

confidence: 99%

Star formation in the S233 region

Ladeyschikov¹,

Соболев²,

Parfenov³

et al. 2015

Mon. Not. R. Astron. Soc.

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“…As for the method to calculate the optical depth, the codes developed so far are basically divided into two categories. the first contains the "neighbor connecting" schemes (Kessel-Deynet & Burkert 2000, Susa & Umemura 2004, Susa 2006, Miao et al 2006, Dale et al 2007, Yoshida et al 2007, Gritschneder et al 2009). In these schemes the optical depth from the point source is assessed utilizing the neighbor lists of SPH particles.…”

Section: Ray-tracingmentioning

confidence: 99%

“…The first one is the "photon conserving method"(Kessel-Deynet & Burkert 2000, Susa 2006, Miao et al 2006, Gritschneder et al 2009) similar to the scheme developed in grid codes (e.g. Abel, Norman & Madau 1999).…”

Section: Photoionization Solvermentioning

confidence: 99%

SPH Radiative Hydrodynamics Methods

Susa

2010

Proc. IAU

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Abstract. In this paper, we review the radiative hydrodynamics methods based upon Smoothed Particle Hydrodynamics(SPH). There are already various implementations so far, which can be categorized into three types: moment equation solvers, Monte Carlo methods, and ray-tracing schemes. These codes have been applied to various astrophysical problems including dynamics of dense proto-stellar cores, photoionization feedback of massive stars on molecular clouds, radiative feedback in the early universe, etc. Among these different methods, we focus on the ray-tracing schemes. We also describe one particular ray-tracing code RSPH in some details.

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“…The signatures of the RDI process are the anisotropic density distribution in a relatively small molecular cloud surrounded by a curved IF (bright rim) as well as a group of young stellar objects (YSOs) aligned from the bright rim towards the direction of the ionizing source(s). Several authors (e.g., Bertoldi 1989;Lefloch & Lazareff 1995;Lefloch et al 1997;De Vries et al 2002;Kessel-Deynet & Burkert 2003;Miao et al 2006) have carried out detailed model calculations of the RDI process. The distribution of YSOs and the morphological details of the environment around massive star(s) are frequently used to probe the star formation history of the region (e.g., Ogura et al 2007;Chauhan et al 2009;Pandey et al 2013a,b, and references therein).…”

Section: Introductionmentioning

confidence: 99%

A multiwavelength investigation of the H ii region S311: young stellar population and star formation

Yadav

Pandey

Sharma

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a multiwavelength investigation of the young stellar population and star formation activities around the H ii region Sharpless 311. Using our deep near-infrared observations and archival Spitzer-IRAC observations, we have detected a total of 125 young stellar objects (YSOs) in an area of ∼86 arcmin 2 . The YSOs sample include 8 Class I and 117 Class II candidate YSOs. The mass completeness of the identified YSOs sample is estimated to be 1.0 M . The ages and masses of the majority of the candidate YSOs are estimated to be in the range of ∼0.1−5 Myr and ∼0.3−6 M , respectively. The 8 µm image of S311 displays an approximately spherical cavity around the ionizing source which is possibly created due to the expansion of the H ii region. The spatial distribution of the candidate YSOs reveals that a significant number of them are distributed systematically along the 8 µm emission with a majority clustered around the eastern border of the H ii region. Four clumps/compact H ii regions are detected in the radio continuum observations at 1280 MHz, which might have been formed during the expansion of the H ii region. The estimated dynamical age of the region, main-sequence lifetime of the ionizing source, the spatial distribution and ages of the candidate YSOs indicate triggered star formation in the complex.

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Triggered star formation in bright-rimmed clouds: the Eagle nebula revisited

Abstract: The definitive version is available at www.blackwell-synergy.com. Copyright Blackwell Publishing DOI : 10.1111/j.1365-2966.2006.10260.

Cited by 90 publications

References 35 publications

Star formation in the S233 region

Star formation in the S233 region

SPH Radiative Hydrodynamics Methods

A multiwavelength investigation of the H ii region S311: young stellar population and star formation

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