Formation of Subsurface Zones in Impact Wear

Rice, Stephen L.; Nowotny, H.; Wayne, Steven F.

doi:10.1080/05698198108983020

Cited by 49 publications

(30 citation statements)

References 9 publications

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“…This dark cloud is located ∼ 120 pc from the main Serpens star-forming regions. The cloud has formed ∼ 15 members bright enough to be identified with Gaia, with a mean distance of 407 pc and a mean proper motion similar to that of Serpens (see also identification of this group by Rice et al 2006). The members of this sub-cluster, including AS 353A (with the associated HH object HH 32 discovered by Mundt et al 1983) and V536 Aql, have similar colors and distance-corrected brightness as those in other Serpens regions.…”

Section: Ldn 673mentioning

confidence: 93%

“…A group of ∼ 15 stars around LDN 673, including AS 353Aab, and a group of 5 stars around FG Aql have proper motions and distances consistent with Serpens membership, but are located ∼ 100 pc away on the sky. These small groups are identified here only because of prior knowledge of their likely youth (Rice et al 2006), and they would otherwise be challenging to detect. Other small groups of 5-20 young stars are likely to be present throughout the Serpens-Aquila field.…”

Section: Searching For Isolated Groups Of Starsmentioning

confidence: 99%

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An Initial Overview of the Extent and Structure of Recent Star Formation within the Serpens Molecular Cloud Using Gaia Data Release 2

Herczeg

Kuhn

Zhou

et al. 2019

ApJ

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The dense clusters within the Serpens Molecular Cloud are among the most active regions of nearby star formation. In this paper, we use Gaia DR2 parallaxes and proper motions to statistically measure ∼ 1167 kinematic members of Serpens, few of which were previously identified, to evaluate the star formation history of the complex. The optical members of Serpens are concentrated in three distinct groups located at 380-480 pc; the densest clusters are still highly obscured by optically-thick dust and have few optical members. The total population of young stars and protostars in Serpens is at least 2000 stars, including past surveys that were most sensitive to protostars and disks, and may be far higher. Distances to dark clouds measured from deficits in star counts are consistent with the distances to the optical star clusters. The Serpens Molecular Cloud is seen in the foreground of the Aquila Rift, dark clouds located at 600-700 pc, and behind patchy extinction, here called the Serpens Cirrus, located at ∼ 250 pc. Based on the lack of a distributed population of older stars, the star formation rate throughout the Serpens Molecular Cloud increased by at least a factor of 20 within the past ∼ 5 Myr. The optically bright stars in Serpens Northeast are visible because their natal molecular cloud has been eroded and not because they were flung outwards from a central factory of star formation. The separation between subclusters of 20-100 pc and the absence of an older population leads to speculation that an external forcing was needed to trigger the active star formation.

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Section: Ldn 673mentioning

confidence: 93%

Section: Searching For Isolated Groups Of Starsmentioning

confidence: 99%

An Initial Overview of the Extent and Structure of Recent Star Formation within the Serpens Molecular Cloud Using Gaia Data Release 2

Herczeg

Kuhn

Zhou

et al. 2019

ApJ

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“…This was later confirmed from the Kband spectroscopy (Tokunaga et al 2004). From the H-band spectroscopy, Rice et al (2006) derived the following parameters for AS 353A: spectral type K5, v sin i = 10 km s −1 , and stellar radial velocity v rad = -11.4 ± 1.1 km s −1 . The stellar bolo-metric luminosity is log(L * /L ) = 0.4 (Tokunaga et al 2004).…”

Section: As 353amentioning

confidence: 73%

“…The star AS 353A belongs to the Aquila star forming region. The distance is estimated as d = 150 ± 50 pc (Prato et al 2003;Rice et al 2006). It is a mixed system with a primary cTTS, AS 353A, and a secondary wTTS, AS 353B.…”

Section: As 353amentioning

confidence: 99%

Line-dependent veiling in very active classical T Tauri stars

Rei

Петров

Gameiro

2018

A&A

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Context. The T Tauri stars with active accretion disks show veiled photospheric spectra. This is supposedly due to non-photospheric continuum radiated by hot spots beneath the accretion shocks at stellar surface and/or chromospheric emission lines radiated by the post-shocked gas. The amount of veiling is often considered as a measure of the mass-accretion rate. Aims. We analysed high-resolution photospheric spectra of accreting T Tauri stars LkHα 321, V1331 Cyg, and AS 353 A with the aim of clarifying the nature of the line-dependent veiling. Each of these objects shows a strong emission line spectrum and powerful wind features indicating high rates of accretion and mass loss. Methods. Equivalent widths of hundreds of weak photospheric lines were measured in the observed spectra of high quality and compared with those in synthetic spectra of appropriate models of stellar atmospheres. Results. The photospheric spectra of the three T Tauri stars are highly veiled. We found that the veiling is strongly line-dependent: larger in stronger photospheric lines and weak or absent in the weakest ones. No dependence of veiling on excitation potential within 0 to 5 eV was found. Different physical processes responsible for these unusual veiling effects are discussed in the framework of the magnetospheric accretion model. Conclusions. The observed veiling has two origins: 1) an abnormal structure of stellar atmosphere heated up by the accreting matter, and 2) a non-photospheric continuum radiated by a hot spot with temperature lower than 10000 K. The true level of the veiling continuum can be derived by measuring the weakest photospheric lines with equivalent widths down to ≈10 mÅ. A limited spectral resolution and/or low signal-to-noise ratio results in overestimation of the veiling continuum. In the three very active stars, the veiling continuum is a minor contributor to the observed veiling, while the major contribution comes from the line-dependent veiling.

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“…L483 is a dark cloud in Aquila Rift, whose distance from the Sun is 200 pc (Jørgensen et al 2002;Rice et al 2006). This cloud is associated with the infrared source IRAS 18148-0440, which is known to be a Class 0 protostar (Fuller et al 1995;Chapman et al 2013).…”

Section: Target Source: L483mentioning

confidence: 99%

Sub-arcsecond Kinematic Structure of the Outflow in the Vicinity of the Protostar in L483

Oya

Sakai

Watanabe

et al. 2018

ApJ

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The bipolar outflow associated with the Class 0 low-mass protostellar source (IRAS 18148-0440) in L483 has been studied in the CCH and CS line emission at 245 and 262 GHz, respectively. Sub-arcsecond resolution observations of these lines have been conducted with ALMA. Structures and kinematics of the outflow cavity wall are investigated in the CS line, and are analyzed by using a parabolic model of an outflow. We constrain the inclination angle of the outflow to be from 75 • to 90 • , i.e. the outflow is blowing almost perpendicular to the line of sight. Comparing the outflow parameters derived from the model analysis with those of other sources, we confirm that the opening angle of the outflow and the gas velocity on its cavity wall correlate with the dynamical timescale of the outflows. Moreover, a hint of a rotating motion of the outflow cavity wall is found.Although the rotation motion is marginal, the specific angular momentum of the gas on the outflow cavity wall is evaluated to be comparable to or twice that of the infalling-rotating envelope of L483.

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Formation of Subsurface Zones in Impact Wear

Cited by 49 publications

References 9 publications

An Initial Overview of the Extent and Structure of Recent Star Formation within the Serpens Molecular Cloud Using Gaia Data Release 2

An Initial Overview of the Extent and Structure of Recent Star Formation within the Serpens Molecular Cloud Using Gaia Data Release 2

Line-dependent veiling in very active classical T Tauri stars

Sub-arcsecond Kinematic Structure of the Outflow in the Vicinity of the Protostar in L483

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