toggle visibility Search & Display Options

Select All    Deselect All
 |   | 
Details
   print
  Record Links
Author (up) Long, F.; Ren, B.B.; Wallack, N.L.; Harsono, D.; Herczeg, G.J.; Pinilla, P.; Mawet, D.; Liu, M.C.; Andrews, S.M.; Bai, X.N.; Cabrit, S.; Cieza, L.A.; Johnstone, D.; Leisenring, J.M.; Lodato, G.; Liu, Y.; Manara, C.F.; Mulders, G.D.; Ragusa, E.; Sallum, S.; Shi, Y.F.; Tazzari, M.; Uyama, T.; Wagner, K.; Wilner, D.J.; Xuan, J.W. doi  openurl
  Title A Large Double-ring Disk Around the Taurus M Dwarf J04124068+2438157 Type
  Year 2023 Publication Astrophysical Journal Abbreviated Journal Astrophys. J.  
  Volume 949 Issue 1 Pages 27  
  Keywords SPECTRAL ENERGY-DISTRIBUTIONS; PRE-MAIN-SEQUENCE; LOW-MASS STARS; ALMA SURVEY; MILLIMETER CONTINUUM; PROTOPLANETARY DISKS; LINE OBSERVATIONS; HOMOGENEOUS ANALYSIS; CIRCUMSTELLAR DISCS; EVOLUTIONARY MODELS  
  Abstract Planet formation imprints signatures on the physical structures of disks. In this paper, we present high-resolution (similar to 50 mas, 8 au) Atacama Large Millimeter/submillimeter Array observations of 1.3 mm dust continuum and CO line emission toward the disk around the M3.5 star 2MASSJ04124068+2438157. The dust disk consists of only two narrow rings at radial distances of 0 47 and 0 78 (similar to 70 and 116 au), with Gaussian sigma widths of 5.6 and 8.5 au, respectively. The width of the outer ring is smaller than the estimated pressure scale height by similar to 25%, suggesting dust trapping in a radial pressure bump. The dust disk size, set by the location of the outermost ring, is significantly larger (by 3 sigma) than other disks with similar millimeter luminosity, which can be explained by an early formation of local pressure bump to stop radial drift of millimeter dust grains. After considering the disk's physical structure and accretion properties, we prefer planet-disk interaction over dead zone or photoevaporation models to explain the observed dust disk morphology. We carry out high-contrast imaging at the L' band using Keck/NIRC2 to search for potential young planets, but do not identify any source above 5 sigma. Within the dust gap between the two rings, we reach a contrast level of similar to 7 mag, constraining the possible planet below similar to 2-4M(Jup). Analyses of the gap/ring properties suggest that an approximately Saturn-mass planet at similar to 90 au is likely responsible for the formation of the outer ring, which can potentially be revealed with JWST.  
  Address  
  Corporate Author Thesis  
  Publisher Place of Publication Editor  
  Language Summary Language Original Title  
  Series Editor Series Title Abbreviated Series Title  
  Series Volume Series Issue Edition  
  ISSN 0004-637X ISBN Medium  
  Area Expedition Conference  
  Notes WOS:000996064100001 Approved  
  Call Number UAI @ alexi.delcanto @ Serial 1828  
Permanent link to this record
Select All    Deselect All
 |   | 
Details
   print

Save Citations:
Export Records: