A chemical map of the outbursting V883 Ori system: vertical and radial structures

Ruíz-Rodríguez, Dary; Williams, Jonathan P.; Kastner, Joel H.; Cieza, Lucas A.; Leemker, M.; Principe, David A.

doi:10.1093/mnras/stac1879

Cited by 7 publications

(3 citation statements)

References 51 publications

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“…The most prominent common feature from the moment 0 maps is the emission hole inside r ∼ 0 1. This feature has already been well recognized in previous ALMA Band 7 observations (Lee et al 2019), and it is caused by optically thick dust continuum emission, which blocks all molecular emission (Lee et al 2019;Ruíz-Rodríguez et al 2022). The emission size varies significantly between molecules: CO (>4″) and HCO + (∼3″) have the largest emission regions, while SO 2 (∼0 5) has the smallest emission size.…”

Section: Spatial Distribution Of Molecular Emissionsupporting

confidence: 59%

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ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). I. What Triggered the Current Episode of Eruption?

Lee,

Kim,

Lee

et al. 2024

ApJ

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An unbiased spectral survey of V883 Ori, an eruptive young star, was carried out with the Atacama Large Millimeter/submillimeter Array in Band 6. The detected line emission from various molecules reveals morphological/kinematical features in both the Keplerian disk and the infalling envelope. A direct infall signature, redshifted absorption against the continuum, has been detected in CO, HCO+, HCN, HNC, and H2CO. HCO+ and SO show large armlike structures that probably connect the infalling envelope to the disk. HCN and H2CO reveal a distinct boundary between the inner and outer disks and tentative spiral structures connecting the outer disk to the inner disk. HNC shows a large central emission hole (r ∼ 0.″3) due to its chemical conversion to HCN at high temperatures. HDO emission, a direct tracer of the water sublimation region, has been detected in the disk. Molecular emission from complex organic molecules is confined within the HDO emission boundary, and HCO+ has an emission hole in its distribution due to its destruction by water. Together, these features suggest that the current episode of eruption in V883 Ori may be triggered by the infall from the envelope to the outer disk, generating a spiral wave that propagates inward and greatly enhances the accretion onto the central star.

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Section: Spatial Distribution Of Molecular Emissionsupporting

confidence: 59%

“…Above all, the complete frequency coverage from ∼221 to ∼275 GHz, with a decent velocity resolution (∼0.6 km s −1 ), allows us to utilize various molecules to explore the different physical/kinematical structures. As a result, our work will complement the investigation by Ruíz-Rodríguez et al (2022).…”

Section: Introductionmentioning

confidence: 60%

ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). I. What Triggered the Current Episode of Eruption?

Lee,

Kim,

Lee

et al. 2024

ApJ

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“…For example, accretion outbursts are known to increase UV flux and disk temperature. Observations and models indicate that outbursts evaporate ices and increase gas density, which in turn drives chemical reactions (e.g., Molyarova et al 2018;Kóspál et al 2021;Leemker et al 2021;Fischer et al 2022;Ruíz-Rodríguez et al 2022;Tobin et al 2023).…”

Section: Introductionmentioning

confidence: 99%

MAPS: Constraining Serendipitous Time Variability in Protoplanetary Disk Molecular Ion Emission

Waggoner,

Cleeves,

Loomis

et al. 2023

ApJ

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Theoretical models and observations suggest that the abundances of molecular ions in protoplanetary disks should be highly sensitive to the variable ionization conditions set by the young central star. We present a search for temporal flux variability of HCO+ J = 1–0, which was observed as a part of the Molecules with Atacama Large Millimeter/submillimeter Array (ALMA) at Planet-forming Scales ALMA Large Program. We split out and imaged the line and continuum data for each individual day the five sources were observed (HD 163296, AS 209, GM Aur, MWC 480, and IM Lup, with between three and six unique visits per source). Significant enhancement (>3σ) was not observed, but we find variations in the spectral profiles in all five disks. Variations in AS 209, GM Aur, and HD 163296 are tentatively attributed to variations in HCO+ flux, while variations in IM Lup and MWC 480 are most likely introduced by differences in the uv coverage, which impact the amount of recovered flux during imaging. The tentative detections and low degree of variability are consistent with expectations of X-ray flare-driven HCO+ variability, which requires relatively large flares to enhance the HCO+ rotational emission at significant (>20%) levels. These findings also demonstrate the need for dedicated monitoring campaigns with high signal-to-noise ratios to fully characterize X-ray flare-driven chemistry.

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The environment around young eruptive stars

Zurlo,

Weber,

Pérez

et al. 2024

A&A

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Eruptive stars are a class of young stellar objects that show an abrupt increase in luminosity. These burst-like episodes are thought to dominate the stellar accretion process during the class 0 to class I stage. We present an overview of a survey of seven episodically accreting protostars carried out to study their potentially complex circumstellar surroundings. The observations were performed with the instrument SPHERE, mounted at the Very Large Telescope. SPHERE is equipped with an extreme adaptive optics system that allows high-contrast imaging. We observed the eruptive stars in the $H$ band with the near-infrared imager IRDIS and used the polarimeter to extract the polarized light scattered from the stars' surroundings. We produced polarized light images for three FUor objects, Z CMa, V960 Mon, and FU Ori, and four EXor objects, XZ Tau, UZ Tau, NY Ori, and EX Lup. We calculated the intrinsic polarization fraction for all the observed stars. In all systems we registered scattered light from around the primary star. FU Ori and V960 Mon are surrounded by complex structures, including spiral-like features. In Z CMa, we detected a point source 0 to the northeast of the primary. Based on the astrometric measurements from archival Keck/NIRC2 data, we find this source to be a third member of the system. Furthermore, Z CMa displays an outflow that extends for thousands of au. Unlike the other EXor objects in our sample, XZ Tau shows bright, extended scattered light structures that are also associated with an outflow on a scale of hundreds of au. The other EXors show relatively faint disk-like structures in the immediate vicinity of the coronagraph. Each object shows a unique environment, but we classified the seven objects into three categories: systems with illuminated outflows, asymmetric arms, and faint disks. Asymmetric arms were only found around FUor objects, while faint disks seem to predominantly occur around EXors. Importantly, for Z CMa the detection of the faint extended structure calls into question previous interpretations of the system's dynamic state. The streamer that was associated with a fly-by object turned out to be part of a huge outflow extending 6000 au.

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A chemical map of the outbursting V883 Ori system: vertical and radial structures

Cited by 7 publications

References 51 publications

ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). I. What Triggered the Current Episode of Eruption?

ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). I. What Triggered the Current Episode of Eruption?

MAPS: Constraining Serendipitous Time Variability in Protoplanetary Disk Molecular Ion Emission

The environment around young eruptive stars

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