PROSAC: a submillimeter array survey of low-mass protostars - II. The mass evolution of envelopes, disks, and stars from the class 0 through I stages

By J. Jørgensen, E. Dishoeck, R. Visser, T. Bourke, D. Wilner, D. Lommen, M. Hogerheijde, P. Myers. 2009

217 citations recorded by the source corpus.

Context. The key question about early protostellar evolution is how matter is accreted from the large-scale molecular cloud, through the circumstellar disk onto the central star. Aims. We constrain the masses of the envelopes, disks, and central stars of a sample of low-mass protostars and compare the results to theoretical models for the evolution of young stellar objects through the early protostellar stages. Methods. A sample of 20 Class 0 and I protostars has been observed in continuum at (sub)millimeter wavelengths at high angular resolution (typically 2 �� ) with the submillimeter array. Using detailed dust radiative transfer models of the interferometric data, as well as single-dish continuum observations, we have developed a framework for disentangling the continuum emission from the envelopes and disks, and from that estimated their masses. For the Class I sources in the sample HCO + 3–2 line emission was furthermore observed with the submillimeter array. Four of these sources show signs of Keplerian rotation, making it possible to determine the masses of the central stars. In the other sources the disks are masked by optically thick envelope and outflow emission. Results. Both Class 0 and I protostars are surrounded by disks with typical masses of about 0.05 M� , although significant scatter is seen in the derived disk masses for objects within both evolutionary stages. No evidence is found for a correlation between the disk . .. . ..

Subfields: Astronomy and Astrophysics, Atmospheric Science, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/d2b2db06380b4f040bea1afbd9245742d241354c

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Citations in the corpus

On the diversity and statistical properties of protostellar discs (2018, background): “Some early studies of Class 0 and I objects inferred masses of unresolved discs ranging from 0.01 to 1.7 M (dust masses 30- 6000 M⊕) with typical masses of 0.05 − 0.2 M (dust masses 200-700 M⊕) (Jørgensen et al. 2009; Enoch et al. 2011).”
A Keplerian disk around a Class 0 source: ALMA observations of VLA1623A (2013, background): “…star formation (Mannings & Sargent 1997; Guilloteau & Dutrey 1998; Guilloteau et al. 1999; Qi et al. 2004; Hughes et al. 2009; Rodriguez et al. 2010), while continuum disk-like structures, the so-called pseudo-disks, are reported in Class 0 objects (Jørgensen et al. 2009; Enoch et al. 2009, 2011).”
RADIATION MAGNETOHYDRODYNAMIC SIMULATIONS OF PROTOSTELLAR COLLAPSE: PROTOSTELLAR CORE FORMATION (2012, background): “Jørgensen et al. (2009) suggested that Class-0 sources (young, embedded) are associated with more massive disks than Class-I sources, which support the early formation of circumstellar disks.”
Protoplanetary Disks and Their Evolution (2011, background): “Recent work demonstrates the possibilities in this area with indications of Keplerian velocity profiles in moderately young, Class I sources (Brinch et al. 2007, Jørgensen et al. 2009, Lommen et al. 2008).”
Our astrochemical heritage (2012, methodology): “After the pioneer work by, e.g., Chandler et al. (1995), Brown et al. (2000) and Looney et al. (2000), further steps toward the characterization of these embedded disks have been made by Jørgensen et al. (2007, 2009), and Enoch et al. (2011).”
NON-IDEAL MHD EFFECTS AND MAGNETIC BRAKING CATASTROPHE IN PROTOSTELLAR DISK FORMATION (2011, background): “…premature to conclude that dense flattened structures observed around deeply embedded protostars (such as from dust continuum observations, e.g., Jørgensen et al. 2009) are rotationally supported disks rather than magnetically induced pseudodisks; the latter can be just as thin as (perhaps even…”
Protostellar disk formation and transport of angular momentum during magnetized core collapse (2012, unknown): “Although as stressed by these authors, these estimates depend on the assumptions made regarding the envelope (Jørgensen et al. 2007, 2009; Enoch et al. 2009, 2011).”
Water in star-forming regions with Herschel (WISH). II. Evolution of 557 GHz 110-101 emission in low-mass protostars (2012, methodology): “The mass estimates presented here fall well within the range of masses derived for these sources using other methods (Bontemps et al. 1996; Hogerheijde et al. 1997, 1998; Chen et al. 2008; Enoch et al. 2009; Jørgensen et al. 2009).”
The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. II. A Statistical Characterization of Class 0 and Class I Protostellar Disks (2020, methodology): “Andersen et al. (2019) utilized Subcompact array data from the SMA with ∼4″ resolution, assumed that the flux density at 50kλ is dominated by the disk, and corrected for the estimated contribution of the envelope at this angular scale (see also Jørgensen et al. 2009).”