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Astronomy Picture of the Day 探索宇宙！每天一幅不同的影像或照片，並由專業天文學家的簡短解釋和說明， 帶你遨遊迷人的宇宙。 2009 年 8 月 5 日 解析參宿四 影像提供: NaCo, VLT, ESO 說明: 這張有史以來最清晰的參宿四 (Betelgeuse)影像顯示，這顆龐大的恆星正緩慢蒸發之中。 A. M. S. Richards, R. J. Davis, L. Decin, S. Etoka, G. M. Harper, J. J. Lim, S. T. Garrington, M. D. Gray, I. McDonald, E. O’Gorman, M. Wittkowski, e-MERLIN resolves Betelgeuse at λ 5 cm: hotspots at 5 R⋆, Monthly Notices of the Royal Astronomical Society: Letters, Volume 432, Issue 1, 15 May 2013, Pages L61–L65, https://doi.org/10.1093/mnrasl/slt036. The 5–6 GHz hotspots, measured at 55–85 mas resolution, have Tb formally above the peak photospheric temperature of 3600 K (Dyck et al. Its proper motion is towards the NE and a bow shock was identified in the infrared (IR) (Noriega-Crespo et al. We used conservative uncertainties, dominated by the maximum uncertainty in the flux scale, although the good agreement with VLA results for the whole-disc flux density suggests that our uncertainties may be overestimated. Betelgeuse (sounds a lot like “beetle juice”), also known as Alpha Orionis, is one of the largest and brightest stars known. This will show whether we are witnessing phenomena propagating outwards smoothly, or localized changes behaving differently, helping to distinguish between convection and pulsation. The above recent image from the >> The peak is 1.116 mJy beam−1. 1.

Kervella/M. Privacy Policy and Important Notices It has an irregular outline but is approximately 100 mas wide, at a radius between ∼175 and 275 mas from the central peak. Betelgeuse (sounds a lot like "beetle juice"), also known as Harper & Brown (2006) studied multi-epoch spatially resolved Hubble Space Telescope (HST) spectra and, by measuring the electron density and comparing it to 22 GHz observations, confirmed the small filling factor. Für die Forscher überraschend: Das Material wurde offenbar nicht von den Polen weggeschleudert, sondern direkt von der Oberfläche des Sterns. Future multifrequency imaging with e-MERLIN, the VLA and ALMA will investigate whether the signatures of chromospheric emission, convection or pulsation shocks are seen in the radio photosphere from 2–10 R⋆, helping to elucidate the mechanisms which eject material from the star into its envelope.

%���� The beam size is (85 × 55) mas2. Die Forscher haben ihn allerdings mit dem NASA-Spezialteleskop für Sonnenbeobachtungen STEREO weiter anvisiert. The total flux density of 1.62–1.71 mJy (depending on whether the SW arc is enclosed) measured at 5.75 GHz, is equivalent to (1.3–1.4) ± 0.2 mJy at 4.85 GHz, using a spectral index of 1.32 (Newell & Hjellming 1982), allowing for the uncertainty in this extrapolation. In 1996, four spots brighter than 0.48 mJy beam−1 (4σrms) were detected, the brightest at 0.56 mJy beam−1. Explodiert der rote Überriese im Sternbild Orion als Supernova? These data sets were reduced using standard techniques (Greisen 1994, Diamond et al.

Betelgeuse Resolved Credit: Pierre Kervella, NaCo, VLT, ESO. Zur optimalen Darstellung unserer Webseite benötigen Sie Javascript. Such speeds are sufficient to supply shock heating even if it is not clear how convection could operate at ≫2.5R⋆. spectacular supernova

The 5.75 GHz photosphere is fitted by a 2D Gaussian component, axes (0.235 × 0.218) arcsec2 (∼5R⋆), flux density 1.62 mJy, with an average brightness temperature ∼1250 K. Extrapolating to 4.9 GHz shows that the flux density decline since 1981 may have levelled off; the large-scale size and brightness is consistent with the results from Lim et al. The residuals after subtracting the central component are shown in the insert of Fig.



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