| DOI | Resolve DOI: https://doi.org/10.1126/science.1248726 |
|---|
| Author | Search for: Dent, W. R. F.; Search for: Wyatt, M. C.; Search for: Roberge, A.; Search for: Augereau, J.-C.; Search for: Casassus, S.; Search for: Corder, S.; Search for: Greaves, J. S.; Search for: De Gregorio-Monsalvo, I.; Search for: Hales, A.; Search for: Jackson, A. P.; Search for: Meredith Hughes, A.; Search for: Lagrange, A.-M.; Search for: Matthews, B.1; Search for: Wilner, D. |
|---|
| Affiliation | - National Research Council of Canada. National Science Infrastructure
|
|---|
| Format | Text, Article |
|---|
| Subject | carbon monoxide; asteroid; carbon monoxide; collision; Mars; molecular analysis; resonance; wavelength; astronomy; attenuation; beta pictoris debris disk; cosmological phenomena; field emission; icy body destruction; moon; planet collision; steady state; velocity |
|---|
| Abstract | Many stars are surrounded by disks of dusty debris formed in the collisions of asteroids, comets, and dwarf planets, but is gas also released in such events? Observations at submillimeter wavelengths of the archetypal debris disk around β Pictoris show that 0.3% of a Moon mass of carbon monoxide orbits in its debris belt. The gas distribution is highly asymmetric, with 30% found in a single clump 85 astronomical units from the star, in a plane closely aligned with the orbit of the inner planet, β Pictoris b. This gas clump delineates a region of enhanced collisions, either from a mean motion resonance with an unseen giant planet or from the remnants of a collision of Mars-mass planets. |
|---|
| Publication date | 2014-03-28 |
|---|
| In | |
|---|
| Language | English |
|---|
| Peer reviewed | Yes |
|---|
| NPARC number | 21272621 |
|---|
| Export citation | Export as RIS |
|---|
| Report a correction | Report a correction (opens in a new tab) |
|---|
| Record identifier | 1f68c87a-f466-4eb8-b729-1ba05a4e7490 |
|---|
| Record created | 2014-12-03 |
|---|
| Record modified | 2020-04-22 |
|---|
