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Sargent, B.; Scherer, D.; Supernok, Y.

doi:10.1007/978-3-663-13305-6_21

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Introduction1

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1994

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“…At this stage, which occurs about 10 6 yr after the onset of proto-stellar collapse, the star is still surrounded by dense circumstellar mll:terial •. possibly in the form of a centrifugally supported accretion disk (for recent observational reviews, see Basri & Bertout 1993;Sargent & Welch 1993). Since such disks are !bought to be the predecessors of planetary systems, detailed mformation on their evolution is warranted.…”

Section: Introductionmentioning

confidence: 99%

Evidence for HCO(+) infall toward T Tauri?

Langevelde¹,

Dishoeck²,

Blake³

1994

ApJ

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H~gh spe~tral and spatial resoluti~n. observations of the Hco+ molecule toward the T Tau binary system obtamed With the Owens Valley Mtlhmeter Array reveal a broad emission line profile (V. = 7 2 km s -1~V = 2.0 km S-1 ) upon ~hie~ a narro~, redshifted absorption feature (VLsR = 8.5 km s-t, AV ~ 0.5 km s-1 ) IS superposed .. one possible InterpretatiOn of the absorption is that it rises from infall of molecular cloud e~velope matenal ont? the i.mmediat~ circumbina~y regio~ •. which would imply that large-scale dynamic accre-!Ion pr~cesses are .~ttll a~tive well mto the optically VISible stages of star formation. Provided the mass IS deposited at radn suff!crently close to the young stars, estimates of the accretion rates indicate that infall may a~d enough matenal to the system to account for the FU Orionis type flares recently observed in T Tau m ~100 yr.

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Section: Introductionmentioning

confidence: 99%