Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 439, Issue 1, Pages 256-263Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stt2405
Keywords
radiative transfer; protoplanetary discs; dust, extinction; infrared: stars
Categories
Funding
- Canada Foundation for Innovation
Ask authors/readers for more resources
We analyse current measurements of accretion rates on to pre-main-sequence stars as a function of stellar mass, and conclude that the steep dependence of accretion rates on stellar mass is real and not driven by selection/detection threshold, as has been previously feared. These conclusions are reached by means of statistical tests including a survival analysis which can account for upper limits. The power-law slope of the (M) over dot-M-* relation is found to be in the range of 1.6-1.9 for young stars with masses lower than 1M(circle dot). The measured slopes and distributions can be easily reproduced by means of a simple disc model which includes viscous accretion and X-ray photoevaporation. We conclude that the (M) over dot - M-* relation in pre-main-sequence stars bears the signature of disc dispersal by X-ray photoevaporation, suggesting that the relation is a straightforward consequence of disc physics rather than an imprint of initial conditions.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available