Alma Observations of the Transition From Infall Motion to Keplerian Rotation Around the Late-Phase Protostar TMC-1a

Aso, Yusuke; Ohashi, Nagayoshi; Saigo, Kazuya; Koyamatsu, Shin; Aikawa, Yuri; Hayashi, Masahiko; Machida, Masahiro N.; Saito, Masao; Takakuwa, Shigehisa; Tomida, Kengo; Tomisaka, Kohji; Yen, Hsi-Wei

doi:10.1088/0004-637x/812/1/27

Cited by 114 publications

(217 citation statements)

References 63 publications

Supporting

Mentioning

183

Contrasting

Order By: Relevance

“…IRAS 04365+2535 is one of the few in our sample with a detected Keplerian rotating disk (e.g., Harsono et al 2014;Aso et al 2015). Our best-fit model for it has a disk with a radius of R 140 au disk and a mass of…”

Section: Iras 04365+2535mentioning

confidence: 94%

“…Harsono et al (2014) observed Keplerian rotation in the IRAS 04365+2535 disk with 13 CO observations and modeled the disk with a radius of 80-100 au and inclination of 55°. Similarly, Aso et al (2015) modeled infall and rotation detected toward the protostar in C 18 O emission and found that the disk has an inclination of 65°and a radius of 100 au. These results are both consistent with our own model fits.…”

Section: Iras 04365+2535mentioning

confidence: 99%

“…It is not clear whether these sources have rotationally supported disks, or whether magnetic braking at these early ages inhibits disk formation (e.g., Allen et al 2003;Mellon & Li 2008;Li et al 2013). Rotationally supported disks have been observed around some Class 0 protostars (Tobin et al 2012(Tobin et al , 2013Murillo et al 2013;Codella et al 2014;Lindberg et al 2014;Aso et al 2015).…”

Section: Introductionmentioning

confidence: 99%

“…They are likely sources with mature protoplanetary disks that are still being fed by a collapsing envelope of material (e.g., Harsono et al 2014;Aso et al 2015).…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Sheehan

Eisner

2017

ApJ

View full text Add to dashboard Cite

Class I protostars are thought to represent an early stage in the lifetime of protoplanetary disks, when they are still embedded in their natal envelope. Here we measure the disk masses of 10 Class I protostars in the Taurus Molecular Cloud to constrain the initial mass budget for forming planets in disks. We use radiative transfer modeling to produce synthetic protostar observations and fit the models to a multi-wavelength data set using a Markov Chain Monte Carlo fitting procedure. We fit these models simultaneously to our new Combined Array for Research in Millimeter-wave Astronomy 1.3 mm observations that are sensitive to the wide range of spatial scales that are expected from protostellar disks and envelopes so as to be able to distinguish each component, as well as broadband spectral energy distributions compiled from the literature. We find a median disk mass of  M 0.018 on average, more massive than the Taurus Class II disks, which have median disk mass of~ M 0.0025 . This decrease in disk mass can be explained if dust grains have grown by a factor of 75 in grain size, indicating that by the Class II stage, at a few Myr, a significant amount of dust grain processing has occurred. However, there is evidence that significant dust processing has occurred even during the Class I stage, so it is likely that the initial mass budget is higher than the value quoted here.

show abstract

Section: Iras 04365+2535mentioning

confidence: 94%

Section: Iras 04365+2535mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

“…They are likely sources with mature protoplanetary disks that are still being fed by a collapsing envelope of material (e.g., Harsono et al 2014;Aso et al 2015).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Disk Masses for Embedded Class I Protostars in the Taurus Molecular Cloud

Sheehan

Eisner

2017

ApJ

View full text Add to dashboard Cite

show abstract

“…Yen et al 2013). The rotation velocity distribution of TMC-1A is given by Aso et al (2015). The radius of the Keplerian disk is about 100 AU and the central star mass is estimated as 0.68M⊙.…”

Section: Tmc-1a (L1534)mentioning

confidence: 99%

The origin of rotation profiles in star-forming clouds

Takahashi

Tomida

Machida

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

Angular momentum distribution and its redistribution are of crucial importance in the formation and evolution of circumstellar disks. Many molecular line observations toward young stellar objects indicate that radial distributions of the specific angular momentum j have a characteristic profile. In the inner region, typically R < ∼ 100 AU, the specific angular momenta distribute like j ∝ r 1/2 , indicating existence of rotationally supported disk. In outer regions, R > ∼ 5000 AU, j increases as the radius increases and the slope is steeper than unity, which is supposed to reflect the original angular momentum distributions in the maternal molecular clouds. In the intermediate region, 100 AU < ∼ R < ∼ 5000AU, j-distribution appears almost flat. While this is often interpreted as a consequence of conservation of the specific angular momentum, the interpretation actually is insufficient and requires a stronger condition that the initial distribution of j must be spatially uniform. However, this requirement seems to be unrealistic and inconsistent with observations. In this work, we propose a simple alternative explanation; the apparently flat j profile is produced by strong elongation due to the large velocity gradient in the accreting flow no matter what the initial j distribution is. To show this we provide a simple analytic model for gravitational collapse of molecular clouds. We also propose a method to estimate ages of protostars using solely the observed rotation profile. We demonstrate its validity in comparison with hydrodynamic simulations, and apply the model to young stellar objects such as L1527 IRS, TMC-1A and B335.

show abstract