ALMA Observations of the HD 110058 Debris Disk

被引:13
|
作者
Hales, Antonio S. [1 ,2 ]
Marino, Sebastian [3 ,4 ,7 ,8 ,9 ]
Sheehan, Patrick D. [2 ,5 ]
Ulloa, Silvio [6 ]
Perez, Sebastian
Matra, Luca [10 ,11 ]
Kral, Quentin [12 ]
Wyatt, Mark [4 ]
Dent, William [1 ,13 ]
Carpenter, John [1 ,2 ]
机构
[1] Joint ALMA Observ, Ave Alonso Cordova 3107, Santiago 7630355, Chile
[2] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA
[3] Univ Cambridge, Jesus Coll, Jesus Lane, Cambridge CB5 8BL, England
[4] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England
[5] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astron, 1800 Sherman Ave, Evanston, IL USA
[6] Univ Chile, Dept Astron, Casilla 36-D, Santiago 8330015, Chile
[7] Univ Santiago Chile, Dept Fis, Estn Cent, Ave Ecuador 3493, Santiago, Chile
[8] Millennium Nucleus Young Exoplanets & Their Moons, Santiago, Chile
[9] Univ Santiago Chile, Ctr Interdisciplinary Res Astrophys & Space Explo, Santiago, Chile
[10] Univ Dublin, Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland
[11] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway H91TK33, Ireland
[12] Univ Paris Diderot, Sorbonne Univ, Univ PSL, Sorbonne Paris Cite,LESIA,Observ Paris,CNRS, 5 Pl Jules Janssen, F-92195 Meudon, France
[13] European Southern Observ, Ave Alonso de Cordova 3107, Santiago 7630355, Chile
来源
ASTROPHYSICAL JOURNAL | 2022年 / 940卷 / 02期
关键词
EXOCOMETARY GAS; BETA-PICTORIS; MOLECULAR GAS; DUST; CO; EVOLUTION; ORIGIN; ASYMMETRIES; PLANET; HOT;
D O I
10.3847/1538-4357/ac9cd3
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the young, gas-rich debris disk around HD 110058 at 0.'' 3-0.'' 6 resolution. The disk is detected in the 0.85 and 1.3 mm continuum, as well as the J = 2-1 and J = 3-2 transitions of (CO)-C-12 and (CO)-C-13. The observations resolve the dust and gas distributions and reveal that this is the smallest debris disk around stars of similar luminosity observed by ALMA. The new ALMA data confirm the disk is very close to edge-on, as shown previously in scattered-light images. We use radiative transfer modeling to constrain the physical properties of dust and gas disks. The dust density peaks at around 31 au and has a smooth outer edge that extends out to similar to 70 au. Interestingly, the dust emission is marginally resolved along the minor axis, which indicates that it is vertically thick if truly close to edge-on with an aspect ratio between 0.13 and 0.28. We also find that the CO gas distribution is more compact than the dust (similar to the disk around 49 Ceti), which could be due to a low viscosity and a higher gas release rate at small radii. Using simulations of the gas evolution taking into account the CO photodissociation, shielding, and viscous evolution, we find that HD 110058's CO gas mass and distribution are consistent with a secondary origin scenario. Finally, we find that the gas densities may be high enough to cause the outward drift of small dust grains in the disk.
引用
收藏
页数:20
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