Dynamical interactions between young stellar objects and a collisional model for the origin of the stellar mass spectrum

Price, Nigel M.; Podsiadlowski, Ph.

doi:10.1093/mnras/273.4.1041

Cited by 44 publications

(38 citation statements)

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“…In a segregated cluster the slope of the massive IMF can be very flat, À $ 0, while at the cluster envelopes it can be as steep as À $ À2:5 (de Grijs et al 2002a). The mechanisms of accretion of peripheral gas (see, e.g., Zinnecker 1982;Myers 2000;Larson 2002;Bonnell et al 2001Bonnell et al , 2004Basu & Jones 2004) and coalescence of other protostars in dense cluster cores (Zinnecker 1986;Larson 1990;Price & Podsiadlowski 1995;Stahler et al 2000;Shadmehri 2004), through which highmass stars can grow by a much larger factor than low-mass stars, make the IMF depend on environment. Coalescence after accretion drag or after accretion-induced cloud core contraction (Bonnell & Bate 2002) also seem likely in dense clusters in view of various simulations (Klessen 2001;Bate et al 2003;Bonnell et al 2003;Gammie et al 2003;Li et al 2003).…”

Section: Introductionmentioning

confidence: 99%

The Low‐Mass Initial Mass Function of the Field Population in the Large Magellanic Cloud withHubble Space TelescopeWFPC2 Observations

Gouliermis¹,

Brandner²,

Henning³

2006

ApJ

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We present V-and I-equivalent HST WFPC2 stellar photometry of an area in the Large Magellanic Cloud (LMC), located to the west of the bar of the galaxy, which accounts for the general background field of its inner disk. The WFPC2 observations reach magnitudes as faint as V ¼ 25 mag, and the large sample of more than 80,000 stars allows us to determine in detail the present-day mass function ( PDMF) of the detected main-sequence stars, which is identical to the initial mass function ( IMF) for masses M P 1 M . The low-mass main-sequence mass function of the LMC field is found not to have a uniform slope throughout the observed mass range; i.e., the slope does not follow a single power law. This slope changes at about 1 M to become more shallow for stars with smaller masses down to the lowest observed mass of $0.7 M , giving clear indications of flattening for even smaller masses. We verified statistically that for stars with M P 1 M the IMF has a slope À around À2, with an indicative slope À ' À1:4 for 0:7 P M /M P 0:9, while for more massive stars the main-sequence mass function becomes much steeper with À ' À5. The main-sequence luminosity function ( LF) of the observed field is in very good agreement with the Galactic LF as it was previously found. Taking into account several assumptions concerning evolutionary effects, which should have changed through time the stellar content of the observed field, we reconstruct qualitatively its IMF for the whole observed mass range (0:7 P M/M P 2:3), and we find that the number of observed evolved stars is not large enough to have affected significantly the form of the IMF, which thus is found almost identical to the observed PDMF.

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Section: Introductionmentioning

confidence: 99%

The Low‐Mass Initial Mass Function of the Field Population in the Large Magellanic Cloud withHubble Space TelescopeWFPC2 Observations

Gouliermis¹,

Brandner²,

Henning³

2006

ApJ

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“…However, this is not the case in the Taurus and the Trapezium populations, which exhibit the same turnover masses of but D0.8 M _ very di †erent low-mass cuto †s of and [0.01 M _ D0.08 respectively. M _ , Theories of the IMF that rely on interactions of cores or protostars (Lejeune & Bastien 1986 ;Murray & Lin 1996 ;Price & Podsiadlowski 1995 ;Bonnell et al 1997) have difficulty in explaining the similarity of the turnover masses in the Trapezium and Taurus, where the stellar densities di †er by 3 orders of magnitude. Dynamical interactions and competitive accretion between protostellar cores were also important in shaping the IMF in numerical modeling of the gravitational collapse and fragmentation of a dense cloud core by Klessen, Burkert, & Matthew (1998).…”

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confidence: 99%

The Initial Mass Function of Low‐Mass Stars and Brown Dwarfs in Taurus

Luhman

2000

ApJ

126

152

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By combining deep optical imaging and infrared spectroscopy with data from the Two-Micron All-Sky Survey (2MASS) and from previous studies (e.g., et al.), I have measured the initial mass funcBricen8 o tion (IMF) for a reddening-limited sample in four Ðelds in the Taurus star-forming region. This IMF is representative of the young populations within these Ðelds for masses above 0.02Relative to the M _ . similarly derived IMF for the Trapezium Cluster (Luhman et al.), the IMF for Taurus exhibits a modest deÐcit of stars above 1 solar mass (i.e., steeper slope), the same turnover mass (D0.8 and a signiÐ-M _ ), cant deÐcit of brown dwarfs. If the IMF in Taurus were the same as that in the Trapezium, 12.8^1.8 brown dwarfs ([0.02 are expected in these Taurus Ðelds where only one brown dwarf candidate is M _ ) found. These results are used to test theories of the IMF.

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“…A sequence of statistical events may naturally lead to a log-normal IMF (see e.g. Zinnecker 1984, Adams & Fatuzzo 1996; also Price & Podsiadlowski 1995, Murray & Lin 1996, Elmegreen 1997.…”

Section: Discussionmentioning

confidence: 99%

“…Now sharing a common environment, these cores compete for the limited reservoir of gas in their surrounding (see e.g. Price & Podsiadlowski 1995, Bonnell et al 1997. Furthermore, the protostellar cores interact gravitationally with each other.…”

Section: The Importance Of Dynamical Interaction and Competitive Accrmentioning

confidence: 99%

Fragmentation in Molecular Clouds: The Formation of a Stellar Cluster

Klessen

Burkert

1999

Interstellar Turbulence

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The isothermal gravitational collapse and fragmentation of a molecular cloud region and the subsequent formation of a protostellar cluster is investigated numerically. The clump mass spectrum which forms during the fragmentation phase can be well approximated by a power law distribution dN/dM ∝ M −1.5 . In contrast, the mass spectrum of protostellar cores that form in the centers of Jeans unstable clumps and evolve through accretion and N -body interaction is best described by a log-normal distribution. Assuming a star formation efficiency of ∼ 10 %, it is in excellent agreement with the IMF of multiple stellar systems.

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Dynamical interactions between young stellar objects and a collisional model for the origin of the stellar mass spectrum

Cited by 44 publications

References 0 publications

The Low‐Mass Initial Mass Function of the Field Population in the Large Magellanic Cloud withHubble Space TelescopeWFPC2 Observations

The Low‐Mass Initial Mass Function of the Field Population in the Large Magellanic Cloud withHubble Space TelescopeWFPC2 Observations

The Initial Mass Function of Low‐Mass Stars and Brown Dwarfs in Taurus

Fragmentation in Molecular Clouds: The Formation of a Stellar Cluster

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