Analysis of information sources in references of the Wikipedia article "Betelgeuse" in English language version.
Assuming a distance of 197±45 pc, an angular distance of 43.33±0.04 mas would equate to a radius of 4.3 AU or 920 R☉
We derive a uniform-disk diameter of 42.05±0.05 mas and a power-law-type limb-darkened disk diameter of 42.49±0.06 mas and a limb-darkening parameter of (9.7±0.5)×10−2
In the article, Lobel et al. equate 1 arcsecond to approximately 40 stellar radii, a calculation which in 2004 likely assumed a Hipparcos distance of 131 pc (430 ly) and a photospheric diameter of 0.0552" from Weiner et al.
{{cite magazine}}: Unknown parameter |agency= ignored (help)[permanent dead link]Images of hotspots on the surface of Betelgeuse taken at visible and infra-red wavelengths using high resolution ground-based interferometers
The 0.047 arcsecond measurement was for a uniform disk. In the article Michelson notes that limb darkening would increase the angular diameter by about 17%, hence 0.055 arcseconds.
The yellow/red "image" or "photo" of Betelgeuse commonly seen is not a picture of the red supergiant, but a mathematically generated image based on the photograph. The photograph was of much lower resolution: The entire Betelgeuse image fit within a 10×10 pixel area on the Hubble Space Telescopes Faint Object Camera. The images were oversampled by a factor of 5 with bicubic spline interpolation, then deconvolved.
Assuming a distance of 197±45 pc, an angular distance of 43.33±0.04 mas would equate to a radius of 4.3 AU or 920 R☉
We derive a uniform-disk diameter of 42.05±0.05 mas and a power-law-type limb-darkened disk diameter of 42.49±0.06 mas and a limb-darkening parameter of (9.7±0.5)×10−2
In the article, Lobel et al. equate 1 arcsecond to approximately 40 stellar radii, a calculation which in 2004 likely assumed a Hipparcos distance of 131 pc (430 ly) and a photospheric diameter of 0.0552" from Weiner et al.
Noriega in 1997 estimated the size to be 0.8 parsecs, having assumed the earlier distance estimate of 400 ly. With a current distance estimate of 643 ly, the bow shock would measure ~1.28 parsecs or over 4 ly
The 0.047 arcsecond measurement was for a uniform disk. In the article Michelson notes that limb darkening would increase the angular diameter by about 17%, hence 0.055 arcseconds.
The yellow/red "image" or "photo" of Betelgeuse commonly seen is not a picture of the red supergiant, but a mathematically generated image based on the photograph. The photograph was of much lower resolution: The entire Betelgeuse image fit within a 10×10 pixel area on the Hubble Space Telescopes Faint Object Camera. The images were oversampled by a factor of 5 with bicubic spline interpolation, then deconvolved.
Assuming a distance of 197±45 pc, an angular distance of 43.33±0.04 mas would equate to a radius of 4.3 AU or 920 R☉
{{cite book}}: |journal= ignored (help)We derive a uniform-disk diameter of 42.05±0.05 mas and a power-law-type limb-darkened disk diameter of 42.49±0.06 mas and a limb-darkening parameter of (9.7±0.5)×10−2
In the article, Lobel et al. equate 1 arcsecond to approximately 40 stellar radii, a calculation which in 2004 likely assumed a Hipparcos distance of 131 pc (430 ly) and a photospheric diameter of 0.0552" from Weiner et al.
Such a major single feature is distinctly different from scattered smaller regions of activity typically found on the Sun although the strong ultraviolet flux enhancement is characteristic of stellar magnetic activity. This inhomogeneity may be caused by a large scale convection cell or result from global pulsations and shock structures that heat the chromosphere."
Noriega in 1997 estimated the size to be 0.8 parsecs, having assumed the earlier distance estimate of 400 ly. With a current distance estimate of 643 ly, the bow shock would measure ~1.28 parsecs or over 4 ly
Photograph showing three of the four enclosures which house 1.8 meter Auxiliary Telescopes (ATs) at the Paranal Observatory in the Atacama Desert region of Chile.
The red giant Betelgeuse is the dimmest seen in years, prompting some speculation that the star is about to explode. Here's what we know.
The 0.047 arcsecond measurement was for a uniform disk. In the article Michelson notes that limb darkening would increase the angular diameter by about 17%, hence 0.055 arcseconds.
The 0.047 arcsecond measurement was for a uniform disk. In the article Michelson notes that limb darkening would increase the angular diameter by about 17%, hence 0.055 arcseconds.
The mysterious dimming of the red supergiant Betelgeuse is the result of a stellar exhalation, astronomers say.
The dramatic dimming of the red supergiant in 2019 was the product of dust, not a prelude to destruction, a new study has found.
The shrinkage corresponds to the star contracting by a distance equal to that between Venus and the Sun, researchers reported June 9 at an American Astronomical Society meeting and in the June 1 Astrophysical Journal Letters.
The 0.047 arcsecond measurement was for a uniform disk. In the article Michelson notes that limb darkening would increase the angular diameter by about 17%, hence 0.055 arcseconds.
Assuming a distance of 197±45 pc, an angular distance of 43.33±0.04 mas would equate to a radius of 4.3 AU or 920 R☉
We derive a uniform-disk diameter of 42.05±0.05 mas and a power-law-type limb-darkened disk diameter of 42.49±0.06 mas and a limb-darkening parameter of (9.7±0.5)×10−2
In the article, Lobel et al. equate 1 arcsecond to approximately 40 stellar radii, a calculation which in 2004 likely assumed a Hipparcos distance of 131 pc (430 ly) and a photospheric diameter of 0.0552" from Weiner et al.
The red giant Betelgeuse is the dimmest seen in years, prompting some speculation that the star is about to explode. Here's what we know.
Images of hotspots on the surface of Betelgeuse taken at visible and infra-red wavelengths using high resolution ground-based interferometers
The shrinkage corresponds to the star contracting by a distance equal to that between Venus and the Sun, researchers reported June 9 at an American Astronomical Society meeting and in the June 1 Astrophysical Journal Letters.
{{cite web}}: CS1 maint: unfit URL (link) Other Versions: "Yowatashi Boshi; Stars that Pass in the Night". Griffith Observer. Vol. 63, no. 10. October 1999. pp. 2–17. and "Yowatashi Boshi; Stars that Pass in the Night". The Kyoto Journal. No. 48. July 2000.