Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1

Añez-López, N.; Osorio, M. R. Zapatero; Busquet, G.; Girart, J. M.; Macías, Enrique; Carrasco-González, Carlos; Curiel, S.; Estalella, R.; Fernández-López, Manuel; Galván-Madrid, Roberto; Kwon, Jungmi; Torrelles, J. M.

doi:10.3847/1538-4357/ab5dbc

Cited by 24 publications

(26 citation statements)

References 91 publications

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“…As in the case of VLA 1, we also adopt a jet inclination angle i =45 • , and estimate lower and upper limits for the mass loss rate considering different approximations for the ionization fraction and the jet velocity, i.e., ∼4×10 −6 M yr −1 (assuming x o = 1 and V jet = 100 km s −1 ) and ∼4×10 −4 M yr −1 (assuming x o = 0.1 and V jet = 1000 km s −1 ), respectively. Such mass-loss rates are significantly higher than those estimated in low-and intermediate-mass YSOs (e.g., Beltrán et al 2001;Anglada, Rodríguez & Carrasco-González 2018), but similar to the values obtained in high-mass YSOs (e.g., Rodríguez et al 1994;Guzmán et al 2012;Añez-López et al 2020), supporting that VLA 3 is excited by a massive protostar.…”

Section: Vlasupporting

confidence: 80%

Characterizing the radio continuum nature of sources in the massive star-forming region W75N (B)

Rodríguez-Kamenetzky

Carrasco-González²,

Torrelles

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT The massive star-forming region W75N (B) is thought to host a cluster of massive protostars (VLA 1, VLA 2, and VLA 3) undergoing different evolutionary stages. In this work, we present radio continuum data with the highest sensitivity and angular resolution obtained to date in this region, using the VLA-A and covering a wide range of frequencies (4–48 GHz), which allowed us to study the morphology and the nature of the emission of the different radio continuum sources. We also performed complementary studies with multi-epoch Very Large Array (VLA) data and Atacama Large Millimeter Array (ALMA) archive data at 1.3 mm wavelength. We find that VLA 1 is driving a thermal radio jet at scales of ≈0.1 arcsec (≈130 au), but also shows signs of an incipient hypercompact H ii region at scales of ≲1 arcsec (≲1300 au). VLA 3 is also driving a thermal radio jet at scales of a few tenths of arcsec (few hundred of au). We conclude that this jet is shock exciting the radio continuum sources Bc and VLA 4 (obscured Herbig–Haro objects), which show proper motions moving outward from VLA 3 at velocities of ≈112–118 km s−1. We have also detected three new weak radio continuum sources, two of them associated with millimetre continuum cores observed with ALMA, suggesting that these two sources are also embedded young stellar objects in this massive star-forming region.

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Section: Vlasupporting

confidence: 80%

Characterizing the radio continuum nature of sources in the massive star-forming region W75N (B)

Rodríguez-Kamenetzky

Carrasco-González²,

Torrelles

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…These observations have been supported by 3D hydrodynamics and radiative transfer calculations, predicting how accretion discs surrounding young high-mass stars form (Bonnell et al 1998;Yorke & Sonnhalter 2002;Krumholz et al 2007;Peters et al 2010;Seifried et al 2011;Harries 2015;Klassen et al 2016;Harries et al 2017;Rosen et al 2019;Ahmadi et al 2019;Añez-López et al 2020). Multiplicity, as an indissociable characteristic of massive star formation, suggests that disc fragmentation can play a crucial role in the formation of the (spectroscopic) companions observed in most systems involving OB stars (Mahy et al 2013;Kobulnicky et al 2014;Chini et al 2012;Kraus et al 2017).…”

Section: Introductionmentioning

confidence: 85%

Parameter study for the burst mode of accretion in massive star formation

Meyer

Vorobyov

Elbakyan

et al. 2020

Monthly Notices of the Royal Astronomical Society

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It is now a widely held view that, in their formation and early evolution, stars build up mass in bursts. The burst mode of star formation scenario proposes that the stars grow in mass via episodic accretion of fragments migrating from their gravitationally-unstable circumstellar discs and it naturally explains the existence of observed pre-main-sequence bursts from high-mass protostars. We present a parameter study of hydrodynamical models of massive young stellar objects (MYSOs) that explores the initial masses of the collapsing clouds (Mc = 60–$200\, \rm M_{\odot }$) and ratio of rotational-to-gravitational energies (β = 0.005 − −0.33). An increase in Mc and/or β produces protostellar accretion discs that are more prone to develop gravitational instability and to experience bursts. We find that all MYSOs have bursts even if their pre-stellar core is such that β ≤ 0.01. Within our assumptions, the lack of stable discs is therefore a major difference between low- and high-mass star formation mechanisms. All our disc masses and disk-to-star mass ratios Md/M⋆ > 1 scale as a power-law with the stellar mass. Our results confirm that massive protostars accrete about 40-60% of their mass in the burst mode. The distribution of time periods between two consecutive bursts is bimodal: there is a short duration ($\sim 1-10~\rm yr$) peak corresponding to the short, faintest bursts and a long-duration peak (at $\sim 10^{3}-10^{4} \rm yr$) corresponding to the long, FU-Orionis-type bursts appearing in later disc evolution, i.e., around $30\, \rm kyr$ after disc formation. We discuss this bimodality in the context of the structure of massive protostellar jets as potential signatures of accretion burst history.

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“…Most disc candidates around high-mass protostars have been observed towards proto-B stars (e.g. Cesaroni et al 2007;Sánchez-Monge et al 2013;Cesaroni et al 2014;Beltrán et al 2014;Beltrán & de Wit 2016;Girart et al 2017;Añez-López et al 2020;Jiménez-Serra et al 2020), with relatively few candidate discs observed towards proto-O stars, e.g. AFGL 2591VLA 3 (Jiménez-Serra et al 2012, NGC 6334 I(N) (Hunter et al 2014), IRAS 16547-4247 (Zapata et al 2015(Zapata et al , 2019, AFGL 4176 (Johnston et al 2015(Johnston et al , 2020, AFGL 2136 (Maud et al 2018(Maud et al , 2019, G11.92-0.61 MM1 (Ilee et al 2016(Ilee et al , 2018, G023.01-0.41 (Sanna et al 2019), G345.50+0.35 M, G345.50+0.35 S and G29.96-0.02 (Cesaroni et al 2017), with central protostellar masses ∼10−45 M and luminosities of (0.1 − 5.8) × 10 5 L .…”

Section: Introductionmentioning

confidence: 99%

ALMA observations of the Extended Green Object G19.01−0.03 – I. A Keplerian disc in a massive protostellar system

Williams

Cyganowski

Brogan

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Using the Atacama Large Millimetre/submillimeter Array (ALMA) and the Karl G. Jansky Very Large Array (VLA), we observed the Extended Green Object (EGO) G19.01–0.03 with sub-arcsecond resolution from 1.05 mm to 5.01 cm wavelengths. Our ∼0.4″ ∼ 1600 AU angular resolution ALMA observations reveal a velocity gradient across the millimetre core MM1, oriented perpendicular to the previously known bipolar molecular outflow, that is consistently traced by 20 lines of 8 molecular species with a range of excitation temperatures, including complex organic molecules (COMs). Kinematic modelling shows the data are well described by models that include a disc in Keplerian rotation and infall, with an enclosed mass of 40 − 70 M⊙ (within a 2000 AU outer radius) for a disc inclination angle of i = 40○, of which 5.4 − 7.2 M⊙ is attributed to the disc. Our new VLA observations show that the 6.7 GHz Class II methanol masers associated with MM1 form a partial ellipse, consistent with an inclined ring, with a velocity gradient consistent with that of the thermal gas. The disc-to-star mass ratio suggests the disc is likely to be unstable and may be fragmenting into as-yet-undetected low mass stellar companions. Modelling the centimetre–millimetre spectral energy distribution of MM1 shows the ALMA 1.05 mm continuum emission is dominated by dust, whilst a free–free component, interpreted as a hypercompact H ii region, is required to explain the VLA ∼5 cm emission. The high enclosed mass derived for a source with a moderate bolometric luminosity (∼104 L⊙) suggests that the MM1 disc may feed an unresolved high-mass binary system.

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Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1

Cited by 24 publications

References 91 publications

Characterizing the radio continuum nature of sources in the massive star-forming region W75N (B)

Characterizing the radio continuum nature of sources in the massive star-forming region W75N (B)

Parameter study for the burst mode of accretion in massive star formation

ALMA observations of the Extended Green Object G19.01−0.03 – I. A Keplerian disc in a massive protostellar system

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