Formation of Planetary-Mass Objects by Protostellar Collapse and Fragmentation

By A. Boss. 2001

133 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/939d2066a4a8660f642763443fb513dc773ccfc3

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

A Universal Stellar Initial Mass Function? A critical look at variations in extreme environments (2010, background): “…mass below which no cluster members exist; this limit would presumably correspond to mass of the smallest clumps in a cloud which can undergo thermal fragmentation (Low & Lynden-Bell 1976; Rees 1976; Spitzer 1978; Boss 2001; Larson 2005; Whitworth et al. 2007; see extended discussion in §4).”
The Stellar Population of the Chamaeleon I Star-forming Region (2007, background): “Several studies have suggested that brown dwarfs form by the ejection of protostellar sources from multiple systems (Reipurth & Clarke 2001; Boss 2001; Bate et al. 2002; Delgado-Donate, Clarke, & Bate 2003; Umbreit et al. 2005; Goodwin & Whitworth 2007).”
Imaging Extrasolar Giant Planets (2016, background): “…theories of planet formation via core accretion and disk instability and may instead represent the tail end of brown dwarf companion formation, perhaps as opacity-limited fragments of turbulent, collapsing molecular cloud cores (e.g., Low & Lynden-Bell 1976; Silk 1977; Boss 2001; Bate 2009).”
The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs (2012, background): “…fragments or protostars in a massive core lead to the ejection of some of them from the core, which prematurely halts their accretion (Bate 2009; Bate & Bonnell 2005; Bate, Bonnell & Bromm 2002, 2003; Boss 2001; Goodwin, Whitworth & Ward-Thompson 2004; Reipurth & Clarke 2001; Umbreit et al. 2005).”
The origin of the initial mass function and its dependence on the mean Jeans mass in molecular clouds (2004, background): “However,theabovem assesareconsistent with the predicted cuto at 1 10 MJ (Low & LyndenBell 1976; Rees 1976; Silk 1977; Boss 1988; M asunaga & Inutsuka 1999;Boss2001).”
MAPPING THE SHORES OF THE BROWN DWARF DESERT. II. MULTIPLE STAR FORMATION IN TAURUS–AURIGA (2011, background): “This process has been modeled extensively for the formation of extrasolar planets (e.g., Boss 2001), but if there is sufficient material left in the disk and envelope, this bound companion would then accrete additional mass and grow into a stellar binary companion (e.g., Clarke 2009).”
Synthetic Spectra and Colors of Young Giant Planet Atmospheres: Effects of Initial Conditions and Atmospheric Metallicity (2008, background): “Since there is some evidence from both observations (Chauvin et al. 2005) and theory (Boss 2001; Kroupa & Bouvier 2003; Ida & Lin 2004) that the “planetary” and “stellar” formation modes may overlap at several Jupiter masses, it will be important to be able to decipher a formation mechanism based…”
Collapse of Rotating Magnetized Molecular Cloud Cores and Mass Outflows (2001, background): “However, a restricted number of articles have been published regarding the dynamical contraction of the cloud with both rotation and magnetic fields (Dorfi 1982, 1989; Basu & Mouschovias 1994, 1995; Boss 2000, 2001); for quasi-static evolution, see Tomisaka, Ikeuchi, & Nakamura (1990).”
New Brown Dwarfs and an Updated Initial Mass Function in Taurus (2004, background): “For instance, Reipurth & Clarke (2001), Boss (2001), and Bate et al. (2002) have suggested that brown dwarfs could form as protostellar sources whose accretion is prematurely halted by ejection from multiple systems.”
Toward a Deterministic Model of Planetary Formation. III. Mass Distribution of Short-Period Planets around Stars of Various Masses (2005, background): “The metallicity dependence on frequency of extrasolar gas giant planets may not be easily accounted for by the gravitational instability scenario, e.g., (Boss 2001), while it is naturally accounted for by the sequential core accretion scenario that we are based on (Paper II).”
The formation of a star cluster: predicting the properties of stars and brown dwarfs (2002, background): “The exact value of the minimum mass is uncertain with theoretical values in the literature ranging from 1− 10 MJ (Low & Lynden-Bell 1976; Silk 1977a; Boss 1988; Masunaga & Inutsuka 1999; Boss 2001).”
Toward a Deterministic Model of Planetary Formation. I. A Desert in the Mass and Semimajor Axis Distributions of Extrasolar Planets (2003, background): “Gas giants could also be formed by self-gravitational collapse of a disk, e.g., (Boss 2001).”