HIDING IN THE SHADOWS. II. COLLISIONAL DUST AS EXOPLANET MARKERS
Abstract
Observations of the youngest planets (∼1–10 Myr for a transitional disk) will increase the accuracy of our planet formation models. Unfortunately, observations of such planets are challenging and time-consuming to undertake, even in ideal circumstances. Therefore, we propose the determination of a set of markers that can preselect promising exoplanet-hosting candidate disks. To this end, N-body simulations were conducted to investigate the effect of an embedded Jupiter-mass planet on the dynamics of the surrounding planetesimal disk and the resulting creation of second-generation collisional dust. We use a new collision model that allows fragmentation and erosion of planetesimals, and dust-sized fragments are simulated in a post-process step including non-gravitational forces due to stellar radiation and a gaseous protoplanetary disk. Synthetic images from our numerical simulations show a bright double ring at 850 μm for a low-eccentricity planet, whereas a high-eccentricity planet would produce a characteristic inner ring with asymmetries in the disk. In the presence of first-generation primordial dust these markers would be difficult to detect far from the orbit of the embedded planet, but would be detectable inside a gap of planetary origin in a transitional disk.
- Authors:
-
- University of Bristol, School of Physics, H. H. Wills Physics Laboratory, University of Bristol, Bristol BS8 1TL (United Kingdom)
- University of Delaware, Department of Physics and Astronomy, 217 Sharp Lab, Newark, DE 19716 (United States)
- University of Bristol, School of Earth Sciences, H. H. Wills Physics Laboratory, University of Bristol, Bristol BS8 1TL (United Kingdom)
- Publication Date:
- OSTI Identifier:
- 22518573
- Resource Type:
- Journal Article
- Journal Name:
- Astrophysical Journal
- Additional Journal Information:
- Journal Volume: 820; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCURACY; ASYMMETRY; COLLISIONS; COMPUTERIZED SIMULATION; COSMIC DUST; EROSION; FRAGMENTATION; IMAGES; JUPITER PLANET; MASS; ORBITS; PROTOPLANETS; STELLAR RADIATION
Citation Formats
Dobinson, Jack, Leinhardt, Zoë M., Lines, Stefan, Carter, Philip J., Dodson-Robinson, Sarah E., and Teanby, Nick A. HIDING IN THE SHADOWS. II. COLLISIONAL DUST AS EXOPLANET MARKERS. United States: N. p., 2016.
Web. doi:10.3847/0004-637X/820/1/29.
Dobinson, Jack, Leinhardt, Zoë M., Lines, Stefan, Carter, Philip J., Dodson-Robinson, Sarah E., & Teanby, Nick A. HIDING IN THE SHADOWS. II. COLLISIONAL DUST AS EXOPLANET MARKERS. United States. https://doi.org/10.3847/0004-637X/820/1/29
Dobinson, Jack, Leinhardt, Zoë M., Lines, Stefan, Carter, Philip J., Dodson-Robinson, Sarah E., and Teanby, Nick A. 2016.
"HIDING IN THE SHADOWS. II. COLLISIONAL DUST AS EXOPLANET MARKERS". United States. https://doi.org/10.3847/0004-637X/820/1/29.
@article{osti_22518573,
title = {HIDING IN THE SHADOWS. II. COLLISIONAL DUST AS EXOPLANET MARKERS},
author = {Dobinson, Jack and Leinhardt, Zoë M. and Lines, Stefan and Carter, Philip J. and Dodson-Robinson, Sarah E. and Teanby, Nick A.},
abstractNote = {Observations of the youngest planets (∼1–10 Myr for a transitional disk) will increase the accuracy of our planet formation models. Unfortunately, observations of such planets are challenging and time-consuming to undertake, even in ideal circumstances. Therefore, we propose the determination of a set of markers that can preselect promising exoplanet-hosting candidate disks. To this end, N-body simulations were conducted to investigate the effect of an embedded Jupiter-mass planet on the dynamics of the surrounding planetesimal disk and the resulting creation of second-generation collisional dust. We use a new collision model that allows fragmentation and erosion of planetesimals, and dust-sized fragments are simulated in a post-process step including non-gravitational forces due to stellar radiation and a gaseous protoplanetary disk. Synthetic images from our numerical simulations show a bright double ring at 850 μm for a low-eccentricity planet, whereas a high-eccentricity planet would produce a characteristic inner ring with asymmetries in the disk. In the presence of first-generation primordial dust these markers would be difficult to detect far from the orbit of the embedded planet, but would be detectable inside a gap of planetary origin in a transitional disk.},
doi = {10.3847/0004-637X/820/1/29},
url = {https://www.osti.gov/biblio/22518573},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 820,
place = {United States},
year = {Sun Mar 20 00:00:00 EDT 2016},
month = {Sun Mar 20 00:00:00 EDT 2016}
}