Abstract
This contribution aims to advance our knowledge of the physical mechanisms driving accretion onto pre-main sequence stars and the dissipation of their circumstellar disks, which are currently not well understood. We present results of a survey of the L1630N and L1641 star-forming clouds in Orion. For a sample of ~400 YSOs we determine their fundamental stellar parameters, disk geometry and accretion rates from a combined data set of optical and infrared photometry and optical spectroscopy. We show that stars residing in clusters or aggregates disperse their disks faster than those formed in isolation, even in very small clusters with low number densities, and in the absence of OB stars. We exclude primordial binarity as a mechanism causing a "transition disk" appearance. We argue that our observations provide observational support for a scenario put forward by Hartmann et al. (2006), in which disks around low-mass stars and brown dwarfs are fully viscous, yielding a steep dependency of the accretion rate on stellar mass of αMaccMαM* 5/2, and stars in the ~solar to intermediate mass regime have substantial dead zones in the disk interior resulting in a shallower relation of approximately αMaccαM*.
| Original language | English |
|---|---|
| Title of host publication | Reviews in Modern Astronomy |
| Subtitle of host publication | Deciphering the Universe through Spectroscopy |
| Editors | Regina von Berlepsch |
| Publisher | Wiley |
| Chapter | 9 |
| Pages | 155-166 |
| Number of pages | 12 |
| Volume | 22 |
| ISBN (Electronic) | 9783527634842 |
| ISBN (Print) | 9783527410552 |
| DOIs | |
| Publication status | Published - 20 Jan 2011 |
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Star and Protoplanetary Disk Properties in Orion's Suburbs. / van Boekel, Roy (Lead / Corresponding author); Fang, Min; Wang, Wei; Carmona, Andrès; Sicilia-Aguilar, Aurora; Henning, Thomas.
Reviews in Modern Astronomy: Deciphering the Universe through Spectroscopy. ed. / Regina von Berlepsch. Vol. 22 Wiley, 2011. p. 155-166.Research output: Chapter in Book/Report/Conference proceeding › Chapter (peer-reviewed)
TY - CHAP
T1 - Star and Protoplanetary Disk Properties in Orion's Suburbs
AU - van Boekel, Roy
AU - Fang, Min
AU - Wang, Wei
AU - Carmona, Andrès
AU - Sicilia-Aguilar, Aurora
AU - Henning, Thomas
PY - 2011/1/20
Y1 - 2011/1/20
N2 - This contribution aims to advance our knowledge of the physical mechanisms driving accretion onto pre-main sequence stars and the dissipation of their circumstellar disks, which are currently not well understood. We present results of a survey of the L1630N and L1641 star-forming clouds in Orion. For a sample of ~400 YSOs we determine their fundamental stellar parameters, disk geometry and accretion rates from a combined data set of optical and infrared photometry and optical spectroscopy. We show that stars residing in clusters or aggregates disperse their disks faster than those formed in isolation, even in very small clusters with low number densities, and in the absence of OB stars. We exclude primordial binarity as a mechanism causing a "transition disk" appearance. We argue that our observations provide observational support for a scenario put forward by Hartmann et al. (2006), in which disks around low-mass stars and brown dwarfs are fully viscous, yielding a steep dependency of the accretion rate on stellar mass of αMaccMαM* 5/2, and stars in the ~solar to intermediate mass regime have substantial dead zones in the disk interior resulting in a shallower relation of approximately αMaccαM*.
AB - This contribution aims to advance our knowledge of the physical mechanisms driving accretion onto pre-main sequence stars and the dissipation of their circumstellar disks, which are currently not well understood. We present results of a survey of the L1630N and L1641 star-forming clouds in Orion. For a sample of ~400 YSOs we determine their fundamental stellar parameters, disk geometry and accretion rates from a combined data set of optical and infrared photometry and optical spectroscopy. We show that stars residing in clusters or aggregates disperse their disks faster than those formed in isolation, even in very small clusters with low number densities, and in the absence of OB stars. We exclude primordial binarity as a mechanism causing a "transition disk" appearance. We argue that our observations provide observational support for a scenario put forward by Hartmann et al. (2006), in which disks around low-mass stars and brown dwarfs are fully viscous, yielding a steep dependency of the accretion rate on stellar mass of αMaccMαM* 5/2, and stars in the ~solar to intermediate mass regime have substantial dead zones in the disk interior resulting in a shallower relation of approximately αMaccαM*.
UR - http://www.scopus.com/inward/record.url?scp=84948968487&partnerID=8YFLogxK
U2 - 10.1002/9783527634842.ch9
DO - 10.1002/9783527634842.ch9
M3 - Chapter (peer-reviewed)
SN - 9783527410552
VL - 22
SP - 155
EP - 166
BT - Reviews in Modern Astronomy
A2 - von Berlepsch, Regina
PB - Wiley
ER -