Massive young disks around Herbig Ae stars

Boissier, J.; Alonso-Albi, T.; Fuente, A.; Berné, O.; Bachiller, R.; Neri, R.; Ginard, D.

doi:10.1051/0004-6361/201016306

Cited by 16 publications

(11 citation statements)

References 54 publications

(96 reference statements)

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“…The protostellar mass of the millimeter brightest FUor-like object, V883 Ori, was constrained to be ∼1.3 M ⊙ by the Keplerian rotation curve of CO gas (Cieza et al 2016), which may be a relatively massive YSO in our sample but not extreme. However, we caution that interpreting the higher millimeter luminosity of the observed FUors/EXors, compared to the M * >1.3 M ⊙ Class II objects, as a consequence of a higher average stellar mass of the FUors/EXors sample, may require extrapolating the correlation between F 353 pc 1.33 mm and M * to a stellar mass beyond the range for which this correlation was measured (c.f., Boissier et al 2011;Andrews et al 2013).…”

Section: Discussionmentioning

confidence: 99%

A 1.3 mm SMA survey of 29 variable young stellar objects

Liu

Dunham

Pascucci

et al. 2018

A&A

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Context. Young stellar objects (YSOs) may undergo periods of active accretion (outbursts), during which the protostellar accretion rate is temporarily enhanced by a few orders of magnitude. Whether or not these accretion outburst YSOs possess similar dust/gas reservoirs to each other, and whether or not their dust/gas reservoirs are similar as quiescent YSOs, are issues not yet clarified. Aims. The aim of this work is to characterize the millimeter thermal dust emission properties of a statistically significant sample of long and short duration accretion outburst YSOs (i.e., FUors and EXors) and the spectroscopically identified candidates of accretion outbursting YSOs (i.e., FUor-like objects). Methods. We have carried out extensive Submillimeter Array (SMA) observations mostly at ∼225 GHz (1.33 mm) and ∼272 GHz (1.10 mm), from 2008 to 2017. We covered accretion outburst YSOs located at <1 kpc distances from the solar system. Results. We analyze all the existing SMA data of such objects, both published and unpublished, in a coherent way to present a millimeter interferometric database of 29 objects. We obtained 21 detections at >3-σ significance. Detected sources except for the two cases of V883 Ori and NGC 2071 MM3 were observed with ∼1 ′′ angular resolution. Overall our observed targets show a systematically higher millimeter luminosity distribution than those of the M * >0.3 M⊙ Class II YSOs in the nearby ( 400 pc) low-mass star-forming molecular clouds (e.g., Taurus, Lupus, Upp Scorpio, and Chameleon I). In addition, at 1 mm our observed confirmed binaries or triple-system sources are systematically fainter than the rest of the sources even though their 1 mm fluxes are broadly distributed. We may have detected ∼30-60% millimeter flux variability from V2494 Cyg and V2495 Cyg, from the observations separated by ∼1 year. Conclusions. 1 Hauyu Baobab Liu et al.: SMA survey towards FU Orionis objects and EXors Fig. 1. SMA images of the observed FUors, EXors, and FUor-like objects. Images are taken at the mean frequency of 224-225 GHz (1.33 mm) if not specifically annotated. Synthesized beam is shown in the bottom left corner of each panel. Color bars are in units of mJy beam −1 . Contours are in steps of 3-σ (c.f. Table 1) if not specifically mentioned. Contours of L1551 IRS 5 are 6 mJy beam −1 (2σ) × [-3, 3, 6, 12, 24, 48]. Contours of Haro 5a/6a IRS are 2.4 mJy beam −1 (1σ) × [-3, 3, 6, 12, 24, 48]. Contours of V883 Ori are 7.6 mJy beam −1 (1σ) × [-3, 3, 6, 12, 24, 48]. Contours of V2775 Ori are 1.9 mJy beam −1 (1σ) × [-3, 3, 6, 12, 24]. Contours of V1647 Ori are 0.66 mJy beam −1 (1σ) × [-3, 3, 6, 12, 24, 48, 96]. Image of NGC 2071 MM3 is presented with a θ maj × θ min =5. ′′ 8×3. ′′ 6 (P.A.=43 • ) synthesized beam to better present its extended envelope; contours are 0.66 mJy beam −1 (1σ) × [-3, 3, 6, 12, 24, 48]. Rectangle and cross in the panel of RNO 1B/1C mark the locations of RNO 1B and 1C quoted from Quanz et al. (2007a); in the panel of SVS 13 they mark Per-emb-44 A and B (Anglada et al. 2004); in the pa...

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Section: Discussionmentioning

confidence: 99%

A 1.3 mm SMA survey of 29 variable young stellar objects

Liu

Dunham

Pascucci

et al. 2018

A&A

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“…the 0.8‐M ⊙ disc around a 3.5‐M ⊙ star; Hamidouche 2010), such cases are rare (e.g. Boissier et al 2011) and the usual assumption is that the circumstellar disc mass is always likely to be less than the stellar mass. While this is almost certainly true later in the evolution of a protostar (e.g.…”

Section: Discussionmentioning

confidence: 99%

Collapse of a molecular cloud core to stellar densities: the formation and evolution of pre-stellar discs

Bate

2011

Monthly Notices of the Royal Astronomical Society

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We report results from radiation hydrodynamical simulations of the collapse of molecular cloud cores to form protostars. The calculations follow the formation and evolution of the first hydrostatic core/disc, the collapse to form a stellar core, and effect of stellar core formation on the surrounding disc and envelope. Past barotropic calculations have shown that rapidly rotating first cores evolve into ‘pre‐stellar discs’ with radii up to ∼100 au that may last thousands of years before a stellar core forms. We investigate how the inclusion of a realistic equation of state and radiative transfer alters this behaviour, finding that the qualitative behaviour is similar, but that the pre‐stellar discs may last 1.5–3 times longer in the more realistic calculations. The masses, radii and lifetimes of the discs increase for initial molecular cloud cores with faster rotation rates. In the most extreme case we model, a pre‐stellar disc with a mass of 0.22 M⊙ and a radius of ≈100 au can form in a 1‐M⊙ cloud and last several thousand years before a stellar core is formed. Such large, massive objects may be imaged using the Atacama Large Millimeter/Submillimeter Array. Fragmentation of these massive discs may also provide an effective route to binary and multiple star formation, before radiative feedback from accretion on to the stellar core can inhibit fragmentation. Once collapse to form a stellar core occurs within the pre‐stellar disc, the radiation hydrodynamical simulations produce qualitatively different behaviour from the barotropic calculations due to the accretion energy released. This drives a shockwave through the circumstellar disc and launches a bipolar outflow even in the absence of magnetic fields.

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“…For intermediate-mass (M * ≈ 2−10 M ) YSOs, i.e. objects in the regime of Herbig Ae/Be stars, typical disk masses are about 0.03 M (Boissier et al 2011;Liu et al 2011). Herbig Ae/Be stars with masses of at least M * ∼ 4 M are sufficiently luminous to be generally detectable in our Herschel maps.…”

Section: Herschel Sensitivity To Circumstellar Mattermentioning

confidence: 97%

Herschelfar-infrared observations of the Carina Nebula complex

Gaczkowski

Preibisch

Ratzka

et al. 2012

A&A

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Context. The Carina Nebula represents one of the largest and most active star forming regions known in our Galaxy. It contains numerous very massive (M > ∼ 40 M ) stars that strongly affect the surrounding clouds by their ionizing radiation and stellar winds. Aims. Our recently obtained Herschel PACS and SPIRE far-infrared maps cover the full area (≈8.7 deg 2 ) of the Carina Nebula complex (CNC) and reveal the population of deeply embedded young stellar objects (YSOs), most of which are not yet visible in the mid-or near-infrared. Methods. We study the properties of the 642 objects that are independently detected as point-like sources in at least two of the five Herschel bands. For those objects that can be identified with apparently single Spitzer counterparts, we use radiative transfer models to derive information about the basic stellar and circumstellar parameters. Results. We find that about 75% of the Herschel-detected YSOs are Class 0 protostars. The luminosities of the Herschel-detected YSOs with SED fits are restricted to values of ≤5400 L , their masses (estimated from the radiative transfer modeling) range from ≈1 M to ≈10 M . Taking the observational limits into account and extrapolating the observed number of Herschel-detected protostars over the stellar initial mass function suggest that the star formation rate of the CNC is ∼0.017 M /year. The spatial distribution of the Herschel YSO candidates is highly inhomogeneous and does not follow the distribution of cloud mass. Rather, most Herschel YSO candidates are found at the irradiated edges of clouds and pillars. The far-infrared fluxes of the famous object η Car are about a factor of two lower than expected from observations with the Infrared Space Observatory obtained 15 years ago; this difference may be a consequence of dynamical changes in the circumstellar dust in the Homunculus Nebula around η Car. Conclusions. The currently ongoing star formation process forms only low-mass and intermediate-mass stars, but no massive (M > ∼ 20 M ) stars. The characteristic spatial configuration of the YSOs provides support to the picture that the formation of this latest stellar generation is triggered by the advancing ionization fronts.

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Massive young disks around Herbig Ae stars

Cited by 16 publications

References 54 publications

A 1.3 mm SMA survey of 29 variable young stellar objects

A 1.3 mm SMA survey of 29 variable young stellar objects

Collapse of a molecular cloud core to stellar densities: the formation and evolution of pre-stellar discs

Herschelfar-infrared observations of the Carina Nebula complex

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