The surface structure and linib-darkening profile of Betelgeuse

Burns, Daniel R.; Baldwin, John E.; Boysen, Roger C.; Haniff, C.; Lawson, P. R.; Mackay, Craig D.; Rogers, John A.; Scott, Tania Ruth; Warner, P. J.; Wilson, Donald M.; Young, J. S.

doi:10.1093/mnras/290.1.l11

Cited by 57 publications

(42 citation statements)

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“…Data reduction was carried out using standard methods in which the power spectrum and bispectrum of the interference fringes were averaged over each dataset (Burns et al 1997). The resulting visibilities had formal fractional errors in the range 2−10% of the values, and the closure phases had typical uncertainties of 5−10 • .…”

Section: Coast Data From 1997mentioning

confidence: 99%

Radiative hydrodynamics simulations of red supergiant stars

Chiavassa

Haubois

Young

et al. 2010

A&A

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Context. The red supergiant (RSG) Betelgeuse is an irregular variable star. Convection may play an important role in understanding this variability. Interferometric observations can be interpreted using sophisticated simulations of stellar convection. Aims. We compare the visibility curves and closure phases obtained from our 3D simulation of RSG convection with CO5BOLD to various interferometric observations of Betelgeuse from the optical to the H band to characterize and measure the convection pattern on this star. Methods. We use a 3D radiative-hydrodynamics (RHD) simulation to compute intensity maps in different filters and thus derive interferometric observables using the post-processing radiative transfer code OPTIM3D. The synthetic visibility curves and closure phases are compared to observations. Results. We provide a robust detection of the granulation pattern on the surface of Betelgeuse in both the optical and the H band based on excellent fits to the observed visibility points and closure phases. We determine that the Betelgeuse surface in the H band is covered by small to medium scale (5−15 mas) convection-related surface structures and a large (≈30 mas) convective cell. In this spectral region, H 2 O molecules are the main absorbers and contribute to both the small structures and the position of the first null of the visibility curve (i.e., the apparent stellar radius).

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Section: Coast Data From 1997mentioning

confidence: 99%

Radiative hydrodynamics simulations of red supergiant stars

Chiavassa

Haubois

Young

et al. 2010

A&A

Self Cite

127

130

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“…In October 1995, Burns et al (1997) used the COAST interferometer at λ = 0.80 μm to observe Betelgeuse and found no asymmetry of the stellar disk itself, but their reconstructed image (their Fig. 4) shows an extension along the northeast-southwest direction (PA ≈ 200 • ), aligned with the NACO plume.…”

Section: Previous High Angular Resolution Observationsmentioning

confidence: 99%

The close circumstellar environment of Betelgeuse

Kervella¹,

Verhoelst

Ridgway

et al. 2009

A&A

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Context. Betelgeuse is one the largest stars in the sky in terms of angular diameter. Structures on the stellar photosphere have been detected in the visible and near-infrared as well as a compact molecular environment called the MOLsphere. Mid-infrared observations have revealed the nature of some of the molecules in the MOLsphere, some being the precursor of dust. Aims. Betelgeuse is an excellent candidate to understand the process of mass loss in red supergiants. Using diffraction-limited adaptive optics (AO) in the near-infrared, we probe the photosphere and close environment of Betelgeuse to study the wavelength dependence of its extension, and to search for asymmetries. Methods. We obtained AO images with the VLT/NACO instrument, taking advantage of the "cube" mode of the CONICA camera to record separately a large number of short-exposure frames. This allowed us to adopt a "lucky imaging" approach for the data reduction, and obtain diffraction-limited images over the spectral range 1.04−2.17 μm in 10 narrow-band filters. Results. In all filters, the photosphere of Betelgeuse appears partly resolved. We identify an asymmetric envelope around the star, with in particular a relatively bright "plume" extending in the southwestern quadrant up to a radius of approximately six times the photosphere. The CN molecule provides an excellent match to the 1.09 μm bandhead in absorption in front of the stellar photosphere, but the emission spectrum of the plume is more difficult to interpret. Conclusions. Our AO images show that the envelope surrounding Betelgeuse has a complex and irregular structure. We propose that the southwestern plume is linked either to the presence of a convective hot spot on the photosphere, or to the rotation of the star.

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“…The first image of a stellar photosphere using the COAST interferometer showed a featureless Betelgeuse (Burns et al, 1997).…”

Section: Imaging Stellar Surfacesmentioning

confidence: 99%

Optical interferometry in astronomy

2003

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Abstract. Here I review the current state of the field of optical stellar interferometry, concentrating on ground-based work although a brief report of space interferometry missions is included. We pause both to reflect on decades of immense progress in the field as well as to prepare for a new generation of large interferometers just now being commissioned (most notably, the CHARA, Keck and VLT Interferometers). First, this review summarizes the basic principles behind stellar interferometry needed by the lay-physicist and general astronomer to understand the scientific potential as well as technical challenges of interferometry. Next, the basic design principles of practical interferometers are discussed, using the experience of past and existing facilities to illustrate important points. Here there is significant discussion of current trends in the field, including the new facilities under construction and advanced technologies being debuted. This decade has seen the influence of stellar interferometry extend beyond classical regimes of stellar diameters and binary orbits to new areas such as mapping the accretion disks around young stars, novel calibration of the Cepheid Period-Luminosity relation, and imaging of stellar surfaces. The third section is devoted to the major scientific results from interferometry, grouped into natural categories reflecting these current developments. Lastly, I consider the future of interferometry, highlighting the kinds of new science promised by the interferometers coming on-line in the next few years. I also discuss the longer-term future of optical interferometry, including the prospects for space interferometry and the possibilities of large-scale ground-based projects. Critical technological developments are still needed to make these projects attractive and affordable. †

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The surface structure and linib-darkening profile of Betelgeuse

Cited by 57 publications

References 0 publications

Radiative hydrodynamics simulations of red supergiant stars

Radiative hydrodynamics simulations of red supergiant stars

The close circumstellar environment of Betelgeuse

Optical interferometry in astronomy

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