WARM HCN IN THE PLANET FORMATION ZONE OF GV TAU N
- Observatorio Astronomico Nacional (OAN,IGN), Apdo 112, E-28803 Alcala de Henares (Spain)
- Centro de Astrobiologia (CSIC/INTA), Laboratory of Molecular Astrophysics, Ctra. Ajalvir km. 4, E-28850 Torrejon de Ardoz (Spain)
The Plateau de Bure Interferometer has been used to map the continuum emission at 3.4 mm and 1.1 mm together with the J = 1{yields}0 and J = 3{yields}2 lines of HCN and HCO{sup +} toward the binary star GV Tau. The 3.4 mm observations did not resolve the binary components, and the HCN J = 1{yields}0 and HCO{sup +} J 1{yields}0 line emissions trace the circumbinary disk and the flattened envelope. However, the 1.1 mm observations resolved the individual disks of GV Tau N and GV Tau S and allowed us to study their chemistry. We detected the HCN 3{yields}2 line only toward the individual disk of GV Tau N, and the emission of the HCO{sup +} 3{yields}2 line toward GV Tau S. Simple calculations indicate that the 3{yields}2 line of HCN is formed in the inner R < 12 AU of the disk around GV Tau N where the HCN/HCO{sup +} abundance ratio is >300. On the contrary, this ratio is <1.6 in the disk around GV Tau S. The high HCN abundance measured in GV Tau N is well explained by photochemical processes in the warm (>400 K) and dense (n > 10{sup 7} cm{sup -3}) disk surface.
- OSTI ID:
- 22047668
- Journal Information:
- Astrophysical Journal Letters, Vol. 754, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 2041-8205
- Country of Publication:
- United States
- Language:
- English
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