Abstract
We present Keck images of the dust disk around β Pictoris at λ = 17.9 μm that reveal new structure in its morphology. Within 1Prime; (19 AU) of the star, the long axis of the dust emission is rotated by more than 10° with respect to that of the overall disk. This angular offset is more pronounced than the warp detected at 3Prime;.5 by the Hubble Space Telescope (HST) and is in the opposite direction. By contrast, the long axis of the emission contours ∼1Prime;.5 from the star is aligned with the HST warp. Emission peaks between 1Prime;.5 and 4Prime; from the star hint at the presence of rings similar to those observed in the outer disk at ∼25″ with the HST Space Telescope Imaging Spectrograph. A deconvolved image strongly suggests that the newly detected features arise from a system of four noncoplanar rings. Bayesian estimates based on the primary image lead to ring radii of 14 ± 1, 28 ± 3, 52 ± 2, and 82 ± 2 AU, with orbital inclinations that alternate in orientation relative to the overall disk and decrease in magnitude with increasing radius. We believe these new results make a strong case for the existence of a nascent planetary system around β Pic.
| Original language | English (US) |
|---|---|
| Journal | Astrophysical Journal |
| Volume | 584 |
| Issue number | 1 II |
| DOIs | |
| State | Published - Feb 10 2003 |
Fingerprint
Keywords
- Circumstellar matter
- Infrared: stars
- Planetary systems: formation
- Planetary systems: protoplanetary disks
- Solar system: formation
ASJC Scopus subject areas
- Space and Planetary Science
Cite this
The inner rings of β Pictoris. / Wahhaj, Z.; Koerner, David W; Ressler, M. E.; Werner, M. W.; Backman, D. E.; Sargent, A. I.
In: Astrophysical Journal, Vol. 584, No. 1 II, 10.02.2003.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - The inner rings of β Pictoris
AU - Wahhaj, Z.
AU - Koerner, David W
AU - Ressler, M. E.
AU - Werner, M. W.
AU - Backman, D. E.
AU - Sargent, A. I.
PY - 2003/2/10
Y1 - 2003/2/10
N2 - We present Keck images of the dust disk around β Pictoris at λ = 17.9 μm that reveal new structure in its morphology. Within 1Prime; (19 AU) of the star, the long axis of the dust emission is rotated by more than 10° with respect to that of the overall disk. This angular offset is more pronounced than the warp detected at 3Prime;.5 by the Hubble Space Telescope (HST) and is in the opposite direction. By contrast, the long axis of the emission contours ∼1Prime;.5 from the star is aligned with the HST warp. Emission peaks between 1Prime;.5 and 4Prime; from the star hint at the presence of rings similar to those observed in the outer disk at ∼25″ with the HST Space Telescope Imaging Spectrograph. A deconvolved image strongly suggests that the newly detected features arise from a system of four noncoplanar rings. Bayesian estimates based on the primary image lead to ring radii of 14 ± 1, 28 ± 3, 52 ± 2, and 82 ± 2 AU, with orbital inclinations that alternate in orientation relative to the overall disk and decrease in magnitude with increasing radius. We believe these new results make a strong case for the existence of a nascent planetary system around β Pic.
AB - We present Keck images of the dust disk around β Pictoris at λ = 17.9 μm that reveal new structure in its morphology. Within 1Prime; (19 AU) of the star, the long axis of the dust emission is rotated by more than 10° with respect to that of the overall disk. This angular offset is more pronounced than the warp detected at 3Prime;.5 by the Hubble Space Telescope (HST) and is in the opposite direction. By contrast, the long axis of the emission contours ∼1Prime;.5 from the star is aligned with the HST warp. Emission peaks between 1Prime;.5 and 4Prime; from the star hint at the presence of rings similar to those observed in the outer disk at ∼25″ with the HST Space Telescope Imaging Spectrograph. A deconvolved image strongly suggests that the newly detected features arise from a system of four noncoplanar rings. Bayesian estimates based on the primary image lead to ring radii of 14 ± 1, 28 ± 3, 52 ± 2, and 82 ± 2 AU, with orbital inclinations that alternate in orientation relative to the overall disk and decrease in magnitude with increasing radius. We believe these new results make a strong case for the existence of a nascent planetary system around β Pic.
KW - Circumstellar matter
KW - Infrared: stars
KW - Planetary systems: formation
KW - Planetary systems: protoplanetary disks
KW - Solar system: formation
UR - http://www.scopus.com/inward/record.url?scp=0042761776&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=0042761776&partnerID=8YFLogxK
U2 - 10.1086/346123
DO - 10.1086/346123
M3 - Article
VL - 584
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1 II
ER -