Bolometric luminosity variations in the luminous blue variable AFGL2298

Clark, J. S.; Crowther, P. A.; Larionov, V. M.; Steele, I. A.; Ritchie, B. W.; Архаров, А. А.

doi:10.1051/0004-6361/200912358

Cited by 58 publications

(74 citation statements)

References 62 publications

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“…3.1, we estimated a mass of ∼20 M and a density of ∼120 cm −3 . The obtained mass is higher than the mass of the nebula around G24 estimated by Clark et al (2003) (∼0.45 M ) and of the nebulae around other LBVs (see Owocki 2006 andClark et al 2009). Thus, we propose that the molecular material located right upon the ring nebula belongs mainly to the molecular shell.…”

Section: The Origin Of the Molecular Shellcontrasting

confidence: 56%

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The molecular gas around the luminous blue variable star G24.73+0.69

Petriella

Paron

Giacani

2012

A&A

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Aims. We study the molecular environment of the luminous blue variable star G24.73+0.69 to investigate the origin of the two infrared shells around this massive star and determine its effects on the surrounding interstellar medium. Methods.We analyze the distribution of the molecular gas using the 13 CO J=1-0 emission extracted from the Galactic Ring Survey. We use near and mid-infrared data from 2MASS and GLIMPSE to identify the young stellar objects in the field.Results. We discover the molecular counterpart to the outer infrared shell around G24.73+0.69.The CO shell was probably blown by the stellar wind of the star mainly during its main sequence phase. We also find molecular gas that corresponds to the inner infrared shell, although its origin remains uncertain. We identify seven young stellar objects within the molecular material, whose birth might have been triggered by the stellar wind of the luminous blue variable star. We suggest that both G24.73+0.69 and the progenitor of the nearby supernova remnant G24.7+0.6 were formed from the same natal cloud and represent the most evolved members of a so far undetected cluster of massive stars.

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Section: The Origin Of the Molecular Shellcontrasting

confidence: 56%

“…Clark et al (2003) quoted log(L /L ) = 5.6 for a distance of 5.2 kpc. Taking a distance of 3.5 kpc, the luminosity drops to log(L /L ) ∼ 5.25, which would make it one of the faintest LBVs yet identified (see for comparison the HR diagram of Clark et al 2009), thus a possible post RSG/YHG object.…”

Section: The Distribution Of the Molecular Gasmentioning

confidence: 99%

The molecular gas around the luminous blue variable star G24.73+0.69

Petriella

Paron

Giacani

2012

A&A

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“…We immediately note in Fig. 13 that LBVs are distributed over a range of luminosities (see also van Genderen 2001;Smith et al 2004;Clark et al 2005Clark et al , 2009aClark et al , 2012bVink 2012). If LBVs arise from the evolution of single stars, the spread in luminosity means that they come from a range of initial masses.…”

Section: When Lbvs Are Sn Progenitors and Their Sn Typesmentioning

confidence: 87%

“…(Groh et al 2012;Hillier et al 2001), WR 102ka (Barniske et al 2008), AG Car Groh et al (2009b;Groh et al, in prep. ), AFGL 2298 (Clark et al 2009a), FMM 362 and Pistol star ), Wray 17-96 (Egan et al 2002), G24.73+0.69 (Clark et al 2009a), [OMN2000] LS1 (Clark et al 2009b), HD 316285 (Hillier et al 1998), HD 160529, HD 168625 andHD 168607 (van Genderen 2001), P Cygni (Najarro 2001;2011, priv. comm.…”

Section: When Lbvs Are Sn Progenitors and Their Sn Typesmentioning

confidence: 99%

Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death

Groh

Meynet

Georgy

et al. 2013

A&A

193

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We investigate the fundamental properties of core-collapse supernova (SN) progenitors from single stars at solar metallicity. For this purpose, we combine Geneva stellar evolutionary models with initial masses of M ini = 20−120 M with atmospheric and wind models using the radiative transfer code CMFGEN. We provide synthetic photometry and high-resolution spectra of hot stars at the pre-SN stage. For models with M ini = 9−20 M , we supplement our analysis using publicly available MARCS model atmospheres of RSGs to estimate their synthetic photometry. We employ well-established observational criteria of spectroscopic classification and find that, depending on their initial mass and rotation, massive stars end their lives as red supergiants (RSG), yellow hypergiants (YHG), luminous blue variables (LBV), and Wolf-Rayet (WR) stars of the WN and WO spectral types. For rotating models, we obtained the following types of SN progenitors:, and RSGs (9 ≤ M ini ≤ 18 M ). For non-rotating models, we found spectral types WO1-, and RSGs (9 ≤ M ini ≤ 20 M ). Our rotating models indicate that SN IIP progenitors are all RSG, SN IIL/b progenitors are 56% LBVs and 44% YHGs, SN Ib progenitors are 96% WN10-11 and 4% WOs, and SN Ic progenitors are all WO stars. We find that the most massive and luminous SN progenitors are not necessarily the brightest ones in a given filter, since this depends on their luminosity, temperature, wind density, and the way the spectral energy distribution compares to a filter bandpass. We find that SN IIP progenitors (RSGs) are bright in the RIJHK S filters and faint in the UB filters. SN IIL/b progenitors (LBVs and YHGs), and SN Ib progenitors (WNs) are relatively bright in optical/infrared filters, while SN Ic progenitors (WOs) are faint in all optical filters. We argue that SN Ib and Ic progenitors from single stars should be undetectable in the available pre-explosion images with the current magnitude limits, in agreement with observational results.

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“…Appendix A: Summary of stellar comparison data to Wd1-5 Crowther et al (2006b); (2) Lefever et al (2007); (3) Searle et al (2008); (4) Markova & Puls (2008); (5) Kaper et al (2006); (6) Clark et al (2012); (7) Groh et al (2009a); (8) Najarro (2001); (9) Groh et al (2009b); (10) Najarro et al (2009); (11) Clark et al (2009b); (12) Bohannan & Crowther (1999); (13) Martins et al (2007). …”

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confidence: 99%

A VLT/FLAMES survey for massive binaries in Westerlund 1

Clark

Ritchie

Najarro

et al. 2014

A&A

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Context. The first soft gamma-ray repeater was discovered over three decades ago, and was subsequently identified as a magnetar, a class of highly magnetised neutron star. It has been hypothesised that these stars power some of the brightest supernovae known, and that they may form the central engines of some long duration gamma-ray bursts. However there is currently no consenus on the formation channel(s) of these objects. Aims. The presence of a magnetar in the starburst cluster Westerlund 1 implies a progenitor with a mass ≥40 M , which favours its formation in a binary that was disrupted at supernova. To test this hypothesis we conducted a search for the putative pre-SN companion.Methods. This was accomplished via a radial velocity survey to identify high-velocity runaways, with subsequent non-LTE model atmosphere analysis of the resultant candidate, Wd1-5. Results. Wd1-5 closely resembles the primaries in the short-period binaries, Wd1-13 and 44, suggesting a similar evolutionary history, although it currently appears single. It is overluminous for its spectroscopic mass and we find evidence of He-and N-enrichement, O-depletion, and critically C-enrichment, a combination of properties that is difficult to explain under single star evolutionary paradigms. We infer a pre-SN history for Wd1-5 which supposes an initial close binary comprising two stars of comparable (∼41 M + 35 M ) masses. Efficient mass transfer from the initially more massive component leads to the mass-gainer evolving more rapidly, initiating luminous blue variable/common envelope evolution. Reverse, wind-driven mass transfer during its subsequent WC Wolf-Rayet phase leads to the carbon pollution of Wd1-5, before a type Ibc supernova disrupts the binary system. Under the assumption of a physical association between Wd1-5 and J1647-45, the secondary is identified as the magnetar progenitor; its common envelope evolutionary phase prevents spin-down of its core prior to SN and the seed magnetic field for the magnetar forms either in this phase or during the earlier episode of mass transfer in which it was spun-up. Conclusions. Our results suggest that binarity is a key ingredient in the formation of at least a subset of magnetars by preventing spin-down via core-coupling and potentially generating a seed magnetic field. The apparent formation of a magnetar in a Type Ibc supernova is consistent with recent suggestions that superluminous Type Ibc supernovae are powered by the rapid spin-down of these objects.

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Bolometric luminosity variations in the luminous blue variable AFGL2298

Cited by 58 publications

References 62 publications

The molecular gas around the luminous blue variable star G24.73+0.69

The molecular gas around the luminous blue variable star G24.73+0.69

Fundamental properties of core-collapse supernova and GRB progenitors: predicting the look of massive stars before death

A VLT/FLAMES survey for massive binaries in Westerlund 1

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