Mass-luminosity relation for massive stars

Vitrichenko, E. A.; Nadyozhin, D. K.; Razinkova, T. L.

doi:10.1134/s1063773707040044

Cited by 23 publications

(23 citation statements)

References 35 publications

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“…where ζ 1,Ṁ = 10 16Ṁ 16 g s −1 is the accretion rate inferred from the X-ray luminosity, and µ = 10 30 µ 30 G cm 3 is the NS magnetic moment. The X-ray luminosity of the non-flaring state can be then derived (Shakura et al 2014): , where s = 2.76 is the power law index of the phenomenological mass-luminosity relation for massive stars (see Vitrichenko et al 2007), v ∞ is the terminal wind velocity of massive stars (typically 1000 km s −1 ), v w is the wind velocity at the NS Bondi radius, and P b is the orbital period. Hence, we adopt M = 18M ⊙ as an reference value (see Fig.…”

Section: Quasi-spherical Accretion Onto An Nsmentioning

confidence: 99%

Identification of two new HMXBs in the LMC: an ∼2013 s pulsar and a probable SFXT

Vasilopoulos

Maitra

Haberl

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We report on the X-ray and optical properties of two high-mass X-ray binary systems located in the Large Magellanic Cloud (LMC). Based on the obtained optical spectra, we classify the massive companion as a supergiant star in both systems. Timing analysis of the X-ray events collected by XMM-Newton revealed the presence of coherent pulsations (spin period ∼2013 s) for XMMU J053108.3-690923 and fast flaring behaviour for XMMU J053320.8-684122. The X-ray spectra of both systems can be modelled sufficiently well by an absorbed power-law, yielding hard spectra and high intrinsic absorption from the environment of the systems. Due to their combined X-ray and optical properties we classify both systems as SgXRBs: the 19 th confirmed X-ray pulsar and a probable supergiant fast X-ray transient in the LMC, the second such candidate outside our Galaxy.

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Section: Quasi-spherical Accretion Onto An Nsmentioning

confidence: 99%

Identification of two new HMXBs in the LMC: an ∼2013 s pulsar and a probable SFXT

Vasilopoulos

Maitra

Haberl

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…No mass-luminosity relationship exists for red giants (Malkov 2007). Hence, we assumed the mass-luminosity relation L ∝ M 2.76 given by Vitrichenko et al (2007) for massive stars and Betelgeuse as a reference for mass and luminosity (M = 15 M and M K = −4.38 mag). Concerning the CO band head, we assumed that the ratio…”

Section: Characteristics Of Sscsmentioning

confidence: 99%

Star formation and jet-induced coronal lines near the core of NGC 1068

Exposito

Gratadour

Clénet

et al. 2011

A&A

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Context. Active galactic nuclei (AGNs) are very luminous galaxies from the ultraviolet (UV) to the far infrared (FIR). To study regions near the core, which are dominated by dust, IR is the perfect spectral range because of the lower optical depth of the dust. However, these galaxies are usually distant, and the structures near the core are faint compared to the central source. High resolution and high contrast are mandatory to study the inner structures of AGNs and better understand the interaction between the central core and its surroundings. Aims. Our goal is to propose an explanation for the coronal lines in our spectra of NGC 1068 at a far distance (few tens of parsec) from the central source inside wave-like structures that we call nodules. Methods. NGC 1068 was observed with NaCo at ESO/VLT, using long-slit spectroscopy at 2.2 μm and 3.5 μm. Reduced spectra were compared to the output of Cloudy, using various ionizing continua: the continuum of the central source, young stars, and radiative shocks caused by the jet. Results. For the first time, thanks to the resolution provided by NaCo, near-IR coronal emission can be precisely associated to structures observable in the IR broad-band images. We found that coronal lines observed in the nodules cannot be caused by photoionization by the central source but are instead caused by a local jet-induced ionizing continuum. In addition, studying the Brackett-γ line (Brγ) and CO 2-0 band head, we deduced a star density within the four nodules (∼800 000 stars) compatible with super star cluster (hereafter SSC) models.

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“…The index ζ 2 has been empirically determined by Vitrichenko et al (2007) to be 2.76 for a stellar mass range of 10-50 M . This ζ 2 value is consistent with the index, 2.26-2.98, given by Maeder (2009) for stellar masses of 9-60 M .…”

Section: Linear Relation Expected From Theoretical Modelmentioning

confidence: 99%

Linear Relation for Wind-Blown Bubble Sizes of Main-Sequence Ob Stars in a Molecular Environment and Implication for Supernova Progenitors

Chen

Zhou

Chu

2013

ApJ

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We find a linear relationship between the size of a massive star's main-sequence bubble in a molecular environment and the star's initial mass: R b ≈ 1.22 M/M − 9.16 pc, assuming a constant interclump pressure. Since stars in the mass range of 8 to 25-30 M will end their evolution in the red supergiant phase without launching a Wolf-Rayet wind, the main-sequence wind-blown bubbles are mainly responsible for the extent of molecular gas cavities, while the effect of the photoionization is comparatively small. This linear relation can thus be used to infer the masses of the massive star progenitors of supernova remnants (SNRs) that are discovered to evolve in molecular cavities, while few other means are available for inferring the properties of SNR progenitors. We have used this method to estimate the initial masses of the progenitors of eight SNRs: Kes 69, Kes 75, Kes 78, 3C 396, 3C 397, HC 40, Vela, and RX J1713−3946.

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Mass-luminosity relation for massive stars

Cited by 23 publications

References 35 publications

Identification of two new HMXBs in the LMC: an ∼2013 s pulsar and a probable SFXT

Identification of two new HMXBs in the LMC: an ∼2013 s pulsar and a probable SFXT

Star formation and jet-induced coronal lines near the core of NGC 1068

Linear Relation for Wind-Blown Bubble Sizes of Main-Sequence Ob Stars in a Molecular Environment and Implication for Supernova Progenitors

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