2014
DOI: 10.1051/0004-6361/201424841
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X-ray emission from an FU Orionis star in early outburst: HBC 722

Abstract: Aims. We conducted the first X-ray observations of the newly erupting FU Ori-type outburst in HBC 722 (V2493 Cyg) with the aim to characterize its X-ray behavior and near-stellar environment during early outburst. Methods. We used data from the XMM-Newton and Chandra X-ray observatories to measure X-ray source temperatures and luminosities as well as the gas column densities along the line of sight toward the source. Results. We report a Chandra X-ray detection of HBC 722 with an X-ray luminosity of L X ≈ 4 × … Show more

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Cited by 12 publications
(14 citation statements)
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“…This may come about if the disturbance of a star's magnetosphere by the inward advance of the disk enhances reconnection. Furthermore, X-rays could be generated by strengthened magnetic fields in the disk (Liebhart et al 2014). However, there has been little theoretical guidance on how FU Ori outbursts affect X-ray production.…”
Section: Discussionmentioning
confidence: 99%
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“…This may come about if the disturbance of a star's magnetosphere by the inward advance of the disk enhances reconnection. Furthermore, X-rays could be generated by strengthened magnetic fields in the disk (Liebhart et al 2014). However, there has been little theoretical guidance on how FU Ori outbursts affect X-ray production.…”
Section: Discussionmentioning
confidence: 99%
“…Our understanding of X-ray emission from FU Ori stars has been based on a small number of studies of individual objects, including FU Ori itself (Skinner et al 2010), HBC 722 (Liebhart et al 2014), V960 Mon (Pooley et al 2015), V1735 Cyg (Skinner et al 2009), L1551 IRS 5 (Bally et al 2003;Schneider et al 2011), and Z CMa (Stelzer et al 2009). Several of these studies have noted particularly high X-ray luminosities compared to what is expected for typical YSOs (e.g., Skinner et al 2009Skinner et al , 2010.…”
Section: Introductionmentioning
confidence: 99%
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“…The cosmic-ray ionization rate is set to a standard value of 5 × 10 −17 s −1 (Dalgarno 2006). X-rays are not included; they have been detected in one T Tauri FUor (Liebhart et al 2014), but X-ray luminosities in embedded protostars remain highly uncertain and are beyond the scope of this work.…”
Section: Chemical Networkmentioning
confidence: 99%
“…The NAP region is also known to host two PMS stars in the FU Ori class: V1057 Cyg and V2493 Cyg. This latter was only known as a Classical T Tauri star (CTTS) named HBC722 before its outburst in 2010, and intensively studied thereafter (Semkov et al 2010, Aspin 2011, Green et al 2011, 2013, Dunham et al 2012, Semkov et al 2012, Liebhart et al 2014, and Lee et al 2015. V1057 Cyg was observed in X-rays (but not detected) by Skinner Fig.…”
Section: Introductionmentioning
confidence: 99%