Bringing VY Canis Majoris Down to Size: An Improved Determination of Its Effective Temperature

@article{Massey2006BringingVC,
  title={Bringing VY Canis Majoris Down to Size: An Improved Determination of Its Effective Temperature},
  author={Philip Massey and Emily M. Levesque and Bertrand Plez},
  journal={The Astrophysical Journal},
  year={2006},
  volume={646},
  pages={1203 - 1208}
}
The star VY CMa is a late-type M supergiant with many peculiarities, mostly related to the intense circumstellar environment due to the star's high mass-loss rate. Claims have been made that would imply that this star is considerably more luminous (L ~ 5 × 105 L☉) and larger (R ~ 2800 R☉) than other Galactic red supergiants (RSGs). Indeed, such a location in the H-R diagram would be well within the "Hayashi forbidden zone," where stars cannot be in hydrostatic equilibrium. These extraordinary… 

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References

SHOWING 1-10 OF 50 REFERENCES

The Effective Temperatures and Physical Properties of Magellanic Cloud Red Supergiants: The Effects of Metallicity

We present moderate-resolution spectrophotometry of 36 red supergiants (RSGs) in the LMC and 37 RSGs in the SMC. Using the MARCS atmosphere models to fit this spectrophotometry, we determine the

The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not as Cool as We Thought

We use moderate-resolution optical spectrophotometry and the new MARCS stellar atmosphere models to determine the effective temperatures of 74 Galactic red supergiants (RSGs). The stars are mostly

THE SPECTRUM OF THE IRREGULAR VARIABLE VY CANIS MAJORIS

V Y Canis Majoris1 is a multiple star system immersed in nebulosity. The bright close pair, AB, has a separation of about O'/7 and a Am of about 1TM5. Since its discovery by van den Bos in 1927 the

High-Resolution, Long-Slit Spectroscopy of VY Canis Majoris: The Evidence for Localized High Mass Loss Events

High spatial and spectral resolution spectroscopy of the OH/IR supergiant VY CMa and its circumstellar ejecta reveals evidence for high mass loss events from localized regions on the star occurring

The Asymmetric Nebula Surrounding the Extreme Red Supergiant Vy Canis Majoris

We present HST/WFPC2 images plus ground-based infrared images and photometry of the very luminous OH/IR star VY Canis Majoris. Our WFPC2 data show a complex distribution of knots and filamentary arcs

Spatially extended K i λ7699 emission in the nebula of VY CMa: kinematics and geometry

Long-slit echelle spectra reveal bright extended emission from the K I λ7699 resonance line the reflection nebula surrounding the extreme red supergiant VY Canis Majoris. The central star has long

The Reddening of Red Supergiants: When Smoke Gets in Your Eyes

Deriving the physical properties of red supergiants (RSGs) depends on accurate corrections for reddening by dust. We use our recent modeling of the optical spectra of RSGs to address this topic.

MERLIN observations of water maser proper motions in VY Canis Majoris

ABSTRA C T MERLIN observations of the 22-GHz water masers in the circumstellar envelope of the supergiant VY CMa show an ellipsoidal distribution with a maximum extent of 700 mas east‐ west and 400

The Last Gasps of VY Canis Majoris: Aperture Synthesis and Adaptive Optics Imagery

We present new observations of the red supergiant VY CMa at 1.25, 1.65, 2.26, 3.08, and 4.8 μm. Two complementary observational techniques were utilized: nonredundant aperture masking on the 10 m

Stellar evolution with rotation XI. Wolf-Rayet star populations at different metallicities

Grids of models of massive stars (M ≥ 20 M� ) with rotation are computed for metallicities Z ranging from that of the Small Magellanic Cloud (SMC) to that of the Galactic Centre. The hydrostatic