Comparing binary systems from rotating parent gas structures with different total masses

Arreaga‐García, Guillermo

doi:10.1007/s10509-017-3028-9

Cited by 7 publications

(6 citation statements)

References 56 publications

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“…There are several processes that have been proposed in the literature to play a role in setting the pristine fragmentation of a core, such as the magnetic field (e. g., Boss et al 2004; Vázquez-Semadeni et al 2005; Hennebelle et al 2011, Commerçon et al 2011; Fontani et al 2016), turbulent support (e. g., Zhang et al 2009, 2015; Wang et al 2011, 2014; Pillai et al 2011, Lu et al 2015), or the rotational-to-gravitational energy (e. g., Arreaga-Garcia 2017, Lim et al 2016). Recently, Palau et al (2014, 2015) have studied the aforementioned processes in a sample of 19 massive dense cores and found that the fragmentation level within cores of 0.1 pc is best correlated with the density structure of the cores, rather than with the non-thermal velocity dispersion (Palau et al 2015) or even the rotational-to-gravitational energy (Palau et al 2014).…”

Section: Discussionmentioning

confidence: 99%

Thermal Jeans Fragmentation within ∼1000 au in OMC-1S

Palau

Zapata

Román-Zúñiga

et al. 2018

ApJ

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We present subarcsecond 1.3 mm continuum ALMA observations towards the Orion Molecular Cloud 1 South (OMC-1S) region, down to a spatial resolution of 74 AU, which reveal a total of 31 continuum sources. We also present subarcsecond 7 mm continuum VLA observations of the same region, which allow to further study fragmentation down to a spatial resolution of 40 AU. By applying a Mean Surface Density of Companions method we find a characteristic spatial scale at ~ 560 AU, and we use this spatial scale to define the boundary of 19 'cores' in OMC-1S as groupings of millimeter sources. We find an additional characteristic spatial scale at ~ 2900 AU, which is the typical scale of the filaments in OMC-1S, suggesting a two-level fragmentation process. We measured the fragmentation level within each core and find a higher fragmentation towards the southern filament. In addition, the cores of the southern filament are also the densest (within 1100 AU) cores in OMC-1S. This is fully consistent with previous studies of fragmentation at spatial scales one order of magnitude larger, and suggests that fragmentation down to 40 AU seems to be governed by thermal Jeans processes in OMC-1S.

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Section: Discussionmentioning

confidence: 99%

Thermal Jeans Fragmentation within ∼1000 au in OMC-1S

Palau

Zapata

Román-Zúñiga

et al. 2018

ApJ

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“…In the past few decades, several studies have been performed to investigate the properties of fragmentation in molecular clouds. These works have concentrated on the study of the physical processes that control fragmentation such as turbulence (Zhang et al 2009(Zhang et al , 2015Pillai et al 2011;Wang et al 2011Wang et al , 2014Lu et al 2015), disk fragmentation (e.g., Adams et al 1989;Kratter et al 2010;Vorobyov & Basu 2010), rotational fragmentation (e.g., Lim et al 2016;Arreaga-García 2017), stellar feedback (e.g., Krumholz et al 2007;Peters et al 2010;Myers et al 2013), and magnetic fields (e.g., Boss 2004;Vázquez-Semadeni et al 2005;Commerçon et al 2011a;Hennebelle et al 2011). On the other hand, a number of studies have found that the fragmentation of dusty cores seems to be related to the density of the cores (e.g., Gutermuth et al 2011;Lombardi et al 2013;Ragan et al 2013; Final reduced data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.…”

Section: Introductionmentioning

confidence: 99%

W51 North: A protocluster emerging out of a thermally inhibited fragmenting cloud

Tang

Zapata

Palau

et al. 2021

A&A

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Context. The fragmentation process in massive star-forming regions is one of the contemporary problems in astrophysics, and several physical processes have been proposed to control the fragmentation including turbulence, magnetic field, rotation, stellar feedback, and gravity. However, the fragmentation process has been poorly studied at small spatial scales well below 1000 AU. Aims. W51 IRS2 is a well-known massive star-forming region whose fragmentation properties have not been thoroughly investigated yet. We aim to use the Atacama Large Millimeter and Submillimeter Array (ALMA) high angular resolution data to identify the fragments in W51 IRS2 and to study the fragmentation properties on a spatial scale of 0.04′′ (200 AU). Methods. We used ALMA data of W51 IRS2 from three projects, which give an angular resolution of 0.028′′ (144 AU) at millimeter wavelengths. The continuum images reveal a significant substructure in an east-west ridge, where both W51 North and W51d2 are embedded. A spectral index map has been generated from the 3 and 1.3 mm high-resolution continuum images. We identified compact fragments by using uv-range constrained 1.3 mm continuum data. A mean surface density of companions (MSDC) analysis has been performed to study the separations between fragments. Results. A total number of 33 continuum sources are identified and 29 out of them are defined as fragments in the surveyed region.The MSDC analysis reveals two breaks corresponding to spatial scales of 1845 and 7346 AU, indicative of a two-level clustering phenomenon, along with a linear regime below 1845 AU, mostly associated with W51 North, whose slope is consistent with the slope for the clustering regime of other cluster-like regions in the Galaxy. Conclusions. The typical masses and separations of the fragments as well as the relation between the density and number of fragments can be explained through a thermal Jeans process operating at high temperatures of 200–400 K, consistent with previous measurements of the temperature in the region, and produced by the nearby massive stars. Therefore, although W51 IRS2 seems to be undergoing a thermally inhibited fragmentation phase, this does not seem to prevent the formation of a protocluster associated with W51 North.

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“…In the past few decades, several studies have been performed to investigate the properties of fragmentation in molecular clouds. These works have concentrated on the study of the physical processes that control fragmentation such as turbulence (Zhang et al 2009Pillai et al 2011;Wang et al 2011Wang et al , 2014, disk fragmentation (e.g., Adams, Ruden & Shu 1989;Kratter et al 2010;Vorobyov & Basu 2010), rotational fragmentation (e.g., Lim et al 2016;Arreaga-García 2017), stellar feedback (e.g., Krumholz et al 2007;Peters et al 2010;Myers et al 2013), and magnetic fields (e.g., Boss 2004;Vázquez-Semadeni, Kim, & Ballesteros-Paredes 2005;Commerçon, Hennebelle & Henning 2011;Hennebelle et al 2011). On the other hand, a number of studies have found that the fragmentation of dusty cores seems to be related to the density of the cores (e.g., Gutermuth et al 2011;Lombardi, Lada & Alves 2013;Ragan, Henning & Beuther 2013;Imara 2015;Lee et al 2015;Mairs et al 2016;Nguyen-Luong et al 2016;Liu et al 2016;Pokhrel et al 2016Pokhrel et al , 2018Hacar, Tafalla & Alves 2017;Mercimek et al 2017;Alfaro & Román-Zúñiga 2018;Li et al 2019;Orkisz et al 2019;Sanhueza et al 2019;Sokol et al 2019;Svoboda et al 2019;Zhang et al 2019), indicating that the fragmentation of cores is consistent with a thermal...…”

Section: Introductionmentioning

confidence: 99%

W51North: A protocluster emerging out of a thermally inhibited fragmenting cloud

Tang,

Palau,

Zapata

et al. 2021

Preprint

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Context. The fragmentation process in massive star-forming regions is one of the contemporary problems in astrophysics, and several physical processes have been proposed to control the fragmentation including turbulence, magnetic field, rotation, stellar feedback, and gravity. However, the fragmentation process has been poorly studied at small spatial scales well below 1000 AU. Aims. W51 IRS2 is a well-known massive star-forming region whose fragmentation properties have not been thoroughly investigated yet. We aim to use the Atacama Large Millimeter and Submillimeter Array (ALMA) high angular resolution data to identify the fragments in W51 IRS2 and to study the fragmentation properties on a spatial scale of 0.04 (200 AU). Methods. We used ALMA data of W51 IRS2 from three projects, which give an angular resolution of 0.028 (144 AU) at millimeter wavelengths. The continuum images reveal a significant substructure in an east-west ridge, where both W51 North and W51d2 are embedded. A spectral index map has been generated from the 3 and 1.3 mm high-resolution continuum images. We identified compact fragments by using uv-range constrained 1.3 mm continuum data. A mean surface density of companions (MSDC) analysis has been performed to study the separations between fragments. Results. A total number of 33 continuum sources are identified and 29 out of them are defined as fragments in the surveyed region.The MSDC analysis reveals two breaks corresponding to spatial scales of 1845 AU and 7346 AU, indicative of a two-level clustering phenomenon, along with a linear regime below 1845 AU, mostly associated with W51 North, whose slope is consistent with the slope for the clustering regime of other cluster-like regions in the Galaxy. Conclusions. The typical masses and separations of the fragments as well as the relation between the density and number of fragments can be explained through a thermal Jeans process operating at high temperatures of 200-400 K, consistent with previous measurements of the temperature in the region, and produced by the nearby massive stars. Therefore, although W51 IRS2 seems to be undergoing a thermally inhibited fragmentation phase, this does not seem to prevent the formation of a protocluster associated with W51 North.

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Comparing binary systems from rotating parent gas structures with different total masses

Cited by 7 publications

References 56 publications

Thermal Jeans Fragmentation within ∼1000 au in OMC-1S

Thermal Jeans Fragmentation within ∼1000 au in OMC-1S

W51 North: A protocluster emerging out of a thermally inhibited fragmenting cloud

W51North: A protocluster emerging out of a thermally inhibited fragmenting cloud

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