Expected FU Ori Outburst Amplitudes from the Optical to the Mid-infrared
Abstract
Disks around young stellar objects (YSOs) consist of material that thermally emits the energy provided by a combination of passive heating from the central star, and active, viscous heating due to mass accretion. FU Ori stars are YSOs with substantially enhanced accretion rates in their inner disk regions. As a disk transitions from standard low-state, to FU Ori-like high-state accretion, the outburst manifests through photometric brightening over a broad range of wavelengths. We present results for the expected amplitudes of the brightening between ∼4000 Å and 8 μm—the wavelength range where FU Ori type outburst events are most commonly detected. Our model consists of an optically thick passive + active steady-state accretion disk with low and high accretion states.
Additional Information
© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received December 2021; Accepted January 2022; Published January 2022. We thank Lee Hartmann and Will Fischer for giving this short contribution a once-over.Attached Files
Published - Hillenbrand_2022p6.pdf
Accepted Version - 2201.01012.pdf
Files
Name | Size | Download all |
---|---|---|
md5:e74a94069dab2781b228e46b0b560aca
|
641.0 kB | Preview Download |
md5:fd2b444485722d1a81fe4cb30ddbc69c
|
734.6 kB | Preview Download |
Additional details
- Eprint ID
- 113011
- Resolver ID
- CaltechAUTHORS:20220119-234007101
- Created
-
2022-01-20Created from EPrint's datestamp field
- Updated
-
2022-01-28Created from EPrint's last_modified field
- Caltech groups
- Astronomy Department