Triggered Star Formation and Young Stellar Population in Bright-Rimmed Cloud Sfo 38

Choudhury, R.; Mookerjea, B.; Bhatt, H. C.

doi:10.1088/0004-637x/717/2/1067

Cited by 34 publications

(49 citation statements)

References 68 publications

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“…Recent studies of a number of star formation sites such as those within the Rosette nebula (e.g. Wang et al ; Schneider et al ), the RCW34 (Bik et al ), or the SFO 38 (Choudhary et al ) have revealed several interesting properties, some of which can be reconciled with the numerical models discussed in this study. Yet in the well‐known MCs such as the Orion and Monoceros, Wilson et al () have reported a systematic increase in the age of stellar populations, indicative of sequential propagation of star formation.…”

Section: Discussionsupporting

confidence: 76%

On the evolution of irradiated turbulent clouds: a comparative study between modes of triggered star formation

Anathpindika

Bhatt

2012

Monthly Notices of the Royal Astronomical Society

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Gas within molecular clouds (MCs) is turbulent and unevenly distributed. Interstellar shocks such as those driven by strong fluxes of ionizing radiation (IR) profoundly affect MCs. While small dense MCs exposed to a strong flux of IR have been shown to implode due to radiationdriven shocks, a phenomenon called radiation-driven implosion, larger MCs, however, are likely to survive this flux, which, in fact, may produce new star-forming sites within these clouds. Here we examine this hypothesis using the smoothed particle hydrodynamics algorithm coupled with a ray-tracing scheme that calculates the position of the ionization front at each time-step. We present results from simulations performed for three choices of IR flux spanning the range of fluxes emitted by a typical B-type star to a cluster of OB-type stars. The extent of photoablation, of course, depends on the strength of the incident flux and a strong flux of IR severely ablates an MC. Consequently, the first star formation sites appear in the dense shocked layer along the edges of the irradiated cloud. Radiation-induced turbulence readily generates dense filamentary structure within the photoablated cloud although several new starforming sites also appear in some of the densest regions at the junctions of these filaments. Prevalent physical conditions within an MC play a crucial role in determining the mode, i.e. filamentary as compared to isolated pockets, of star formation, the time-scale on which stars form and the distribution of stellar masses. The probability distribution functions derived for irradiated clouds in this study are intriguing due to their resemblance with those presented in a recent census of irradiated MCs. Furthermore, irrespective of the nature of turbulence, the protostellar mass functions(MFs) derived in this study follow a power-law distribution. When turbulence within the cloud is driven by a relatively strong flux of IR such as that emitted by a massive O-type star or a cluster of such stars, the MF approaches the canonical form due to Salpeter and even turns over for protostellar masses smaller than ∼0.2 M .

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Section: Discussionsupporting

confidence: 76%

On the evolution of irradiated turbulent clouds: a comparative study between modes of triggered star formation

Anathpindika

Bhatt

2012

Monthly Notices of the Royal Astronomical Society

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“…Figure 5 illustrates the SED of the CLASS I and CLASS II sources of the sample. Based on the SED fitting, all the sample sources indicate masses of < 5 M ⊙ and ages of < 3 Myr, which is in good accordance with the results of Nakano et al (2012) and Choudhury et al (2010). Reach et al (2009).…”

Section: Classification Based On Sed Fittingsupporting

confidence: 84%

Sequential clustering of star formations in IC 1396

Huang¹,

Li²

2013

Res. Astron. Astrophys.

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We present in this paper a comprehensive study of the H II region IC 1396 and its star formation activity, in which multi-wavelength data ranging from the optical to the near-and far-infrared were employed. The surface density distribution of all the 2MASS sources with certain detection toward IC 1396 indicates the existence of a compact cluster spatially consistent with the position of the exciting source of the H II region, HD 206267. The spatial distribution of the infrared excessive emission sources selected based on archived 2MASS data reveals the existence of four sub-clusters in this region. One is in association with the open cluster Trumpler 37. The other three are found to be spatially coincident with the bright rims of the H II region. All the excessive emission sources in the near infrared are cross-identified with the AKARI IRC data, an analysis of the spectral energy distributions (SEDs) of the resultant sample leads to the identification of 8 CLASS I, 15 CLASS II and 15 CLASS III sources in IC 1396. Optical identification of the sample sources with R magnitudes brighter than 17 mag corroborates the results from the SED analysis. Based on the spatial distribution of the infrared young stellar objects at different evolutionary stages, the surrounding sub-clusters located in the bright rims are believed to be younger than the central one. This is consistent with a scenario of sequential star formation in this region. Imaging data of a dark patch in IC 1396 by Herschel SPIRE, on the other hand, indicate the presence of two far-infrared cores in LDN 1111, which are likely new generation protostellar objects in formation. So we infer that the star formation process in this H II region was not continuous but episodic.

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“…The size of the symbol denotes the age. We also show the position of Spitzer Class 0/I protostars (green diamonds) as found by Reach et al (2009, top panel) and Choudhury et al (2010, bottom panel). The dashed line in the bottom panel shows the footprint of the Spitzer data.…”

Section: Discussionmentioning

confidence: 82%

T Tauri candidates and accretion rates using IPHAS: method and application to IC 1396

Barentsen¹,

Vink²,

Drew³

et al. 2011

Monthly Notices of the Royal Astronomical Society

104

166

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The Isaac Newton Telescope (INT) Photometric H‐Alpha Survey (IPHAS) is a 1800 deg2 survey of the Northern Galactic Plane, reaching down to r′∼ 21. We demonstrate how the survey can be used to (1) reliably select classical T Tauri star candidates and (2) constrain the mass accretion rates with an estimated relative uncertainty of 0.6 dex. IPHAS is a necessary addition to spectroscopic surveys because it allows large and uniform samples of accretion rates to be obtained with a precise handle on the selection effects. We apply the method on a region of 7 deg2 towards the H ii region IC 1396 in Cepheus OB2 and identify 158 pre‐main‐sequence candidates with masses between 0.2 and 2.0 M⊙ and accretion rates between 10−9.2 and 10−7.0 M⊙ yr−1. We find a power‐law dependency between the stellar mass and the accretion rates with a slope of α= 1.1 ± 0.2, which is less steep than indicated by previous studies. We discuss the influence of method‐dependent systematic effects on the determination of this relationship. The majority of our sample consists of faint, previously unknown, low‐mass T Tauri candidates (56 per cent between 0.2 and 0.5 M⊙). Many candidates are clustered in front of three bright‐rimmed molecular clouds, which are being ionized by the massive star HD 206267 (O6.5V). We discover a spatio‐temporal gradient of increasing accretion rates, increasing Spitzer infrared excess, and younger ages away from the ionizing star, providing a strong indication that the formation of these clusters has been sequentially triggered by HD 206267 during the last ∼1 Myr.

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Triggered Star Formation and Young Stellar Population in Bright-Rimmed Cloud Sfo 38

Cited by 34 publications

References 68 publications

On the evolution of irradiated turbulent clouds: a comparative study between modes of triggered star formation

On the evolution of irradiated turbulent clouds: a comparative study between modes of triggered star formation

Sequential clustering of star formations in IC 1396

T Tauri candidates and accretion rates using IPHAS: method and application to IC 1396

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