Astrophys. J., 631, 1180-1190 (2005/October-1)
Formation and evolution of planetary systems: upper limits to the gas mass in HD 105.
HOLLENBACH D., GORTI U., MEYER M., KIM J.S., MORRIS P., NAJITA J., PASCUCCI I., CARPENTER J., RODMANN J., BROOKE T., HILLENBRAND L., MAMAJEK E., PADGETT D., SODERBLOM D., WOLF S. and LUNINE J.
Abstract (from CDS):
We report infrared spectroscopic observations of HD 105, a nearby (∼40 pc) and relatively young (∼30 Myr) G0 star with excess infrared continuum emission, which has been modeled as arising from an optically thin circumstellar dust disk with an inner hole of size ≳13 AU. We have used the high spectral resolution mode of the Infrared Spectrometer (IRS) on the Spitzer Space Telescope to search for gas emission lines from the disk. The observations reported here provide upper limits to the fluxes of H2S(0) 28 µm, H2S(1) 17 µm, H2S(2) 12 µm, [Fe II] 26 µm, [Si II] 35 µm, and [S I] 25 µm infrared emission lines. The H2line upper limits place direct constraints on the mass of warm molecular gas in the disk: M(H2)<4.6, 3.8x10–2, and 3.0x10–3 MJat T=50, 100, and 200 K, respectively. We also compare the line flux upper limits to predictions from detailed thermal/chemical models of various gas distributions in the disk. These comparisons indicate that if the gas distribution has an inner hole with radius r_i,gas_, the surface density at that inner radius is limited to values ranging from ≲3 g/cm2 at ri,gas=0.5 AU to 0.1 g/cm2 at ri,gas=5-20 AU. These values are considerably below the value for a minimum mass solar nebula, and suggest that less than 1 Jupiter mass (MJ) of gas (at any temperature) exists in the 1-40 AU planet-forming region. Therefore, it is unlikely that there is sufficient gas for gas giant planet formation to occur in HD 105 at this time.
Infrared: Stars - Stars: Planetary Systems: Formation - Planets and Satellites: Formation - Solar System: Formation - stars: individual (HD 105)
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