High sensitivity search for molecular gas in the beta ;Pic disk. On the low gas-to-dust mass ratio of the circumstellar disk around beta PIC toris

Details High sensitivity search for molecular gas in the beta ;Pic disk. On the low gas-to-dust mass ratio of the circumstellar disk around beta PIC toris High sensitivity search for molecular gas in the beta ;Pic disk. On the low gas-to-dust mass ratio of the circumstellar disk around beta PIC toris

Jun 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...334..935l&link_type=abstract

Astronomy and Astrophysics, v.334, p.935-942 (1998)

Astronomy and Astrophysics

Astrophysics

25

Stars: Individual: Beta Pic Toris, Stars: Formation, Stars: Evolution, Stars: Circumstellar Matter, Stars: Planetary Systems, Radio Lines: Stars

Scientific paper

We report on high sensitivity observations of the beta Pic system in four molecular transitions with the 15 m Sest, tracing carbon, silicon and sulphur bearing species (CO, SiO and CS) and, as such, the gaseous component of the circumstellar disk. The lack of signal in the CO (2-1) line is consistent with an interstellar value of CO/H and a very low column density of hydrogen gas [N(H) < 10(19) cm(-2) ]. The data do not require that CO is severely depleted with respect to hydrogen. Rather, we find that the gas-to-dust mass ratio in the disk is abnormally low, viz. m_gas/m_dust < 0.1 (<0.05 at the 1 sigma level), implying an upper limit to the mass of hydrogen gas m(H) < 2 \powten{-2} M_⊕ (5 M_Moon). Evidently, any nebular disk gas from the formation stage of beta Pic has been consumed in planet formation and/or blown out during the early mass loss history of the system. The sensitive search for SiO gas, believed to be presently produced in evaporative grain-grain collisions, gave likewise negative results. From the modeling of the line emission from the beta Pic disk we deduce that this non-detection could be explained by insufficient filling of the Sest beam and that the testing of the theory has to await the advent of the new generation of millimeter interferometers in the southern hemisphere. Based on observations collected with the Swedish \eso\ Submillimeter Telescope, \sest, in La Silla, Chile.

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