Molecular line observations of southern main-sequence stars with dust disks: alpha PS A, beta Pic, epsilon ERI and HR 4796 A. Does the low gas content of the beta PIC and varepsilon ERI disks hint of planets?

Details Molecular line observations of southern main-sequence stars with dust disks: alpha PS A, beta Pic, epsilon ERI and HR 4796 A. Does the low gas content of the beta PIC and varepsilon ERI disks hint of planets? Molecular line observations of southern main-sequence stars with dust disks: alpha PS A, beta Pic, epsilon ERI and HR 4796 A. Does the low gas content of the beta PIC and varepsilon ERI disks hint of planets?

Aug 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...348..133l&link_type=abstract

Astronomy and Astrophysics, v.348, p.133-138 (1999)

Astronomy and Astrophysics

Astrophysics

20

Stars: Individual: Varepsilon Eri, Stars: Formation, Stars: Evolution, Stars: Circumstellar Matter, Stars: Planetary Systems, Radio Lines: Stars

Scientific paper

The results of molecular line observations with the 15 m Sest(star ) of southern Vega-excess stars are presented. The stars alpha Ps A, varepsilon Eri and HR 4796 A were observed in the CO (1-0) and (2-1) lines and beta Pic was observed in the vibrational ground state of SiO, in the (2-1) and (5-4) transitions. In spite of considerably more sensitive observations than in previous attempts, none of these systems was detected with the Sest. We use theoretical models of stellar atmospheres, of the structure and chemistry of interface regions (Pdr s) and of molecular excitation in Keplerian disks of gas and dust to analyze these observational results. Among the observed objects, the K2 V star varepsilon Eri appears particularly suitable and the analysis focusses on this system. A disk model with simple geometry is capable of explaining recent dust continuum observations. Applying this model to the associable molecular gas leads to the conclusion that it is most likely that the disk/ring around varepsilon Eri is largely devoid of any gas (m_gas/m_dust less than 10^{-3} of the interstellar value), presumably due to consumption during planetary system formation. We propose that varepsilon Eri should be a prime candidate for searches for extrasolar planets. In the beta Pic disk, the gas content may be as low, or even lower, as for varepsilon Eri which could be taken as indirect support of the suggested existence of a planetary system associated with this star. Based on observations collected with the Swedish Eso Submillimetre Telescope, Sest, in La Silla, Chile.

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