When the images from the two end mirrors are superimposed in the field of the telescope, a pattern of interference fringes is created. Michelson's Beam Interferometer measures the diameter of Betelgeuse (1920) It is important to remember that direct interferometer measurements can only be used with large stars. What do you think the color of a star indicates about its temperature? Observations by the observers of the AAVSO indicate that Betelgeuse probably reached magnitude 0.2 in 1933 and again in 1942. But they also acknowledge that there’s another possibility to explain rapidly-rotating red supergiants like Betelgeuse. Although a challenge to observe, it is encouraging that Betelgeuse is so bright and easy to find. There are four groups of semiregular variables (SRa, b, c, and d). Karla Thompson – @karlaii / https://www.youtube.com/channel/UCEItkORQYd4Wf0TpgYI_1fw Since both conform to the BeSS standard perhaps this should not be too difficult ? https://www.amazon.com/Universe-Today-Ultimate-Viewing-Cosmos/dp/1624145442/, Audio Podcast version: The point I was making at the time was that V magnitude is not a good indicator of total luminosity in cool stars and the claims in the popular press around that time that Betelgeuse had become less than half as luminous as normal were a gross exaggeration. I see there is now a recent H,J point in the AAVSO database (The first for over a year). It is a distinctly reddish semiregular variable star whose apparent magnitude, varying between +0.0 and +1.6, has the widest range displayed by any first-magnitude star. What does the graph show about the relationship of a star’s color and temperature? Betelgeuse was selected as the first test object since theoretical calculations had suggested that the star was unusually great in size. Perhaps you could point interested parties there. I made a casual comment about the B-V colour curve in that webinar as being, perhaps, indicative of a hotter companion and was rather startled when Tom Calderwood drew my attention to papera by Karovska and others postulating at least one companion. I was alerted by James Foster on the ARAS forum to possible changes in the strength of the H alpha absorption line. I concurr, many of the M and Carbon stars I observe with the Alpy600 are rather inconspicuious, but very prominent in my LISA-IR spectra; sometimes the carbon stars have almost no continuum shorter than 5500A! (These were uploaded as Visual and IR spectra to the AASVO spectra database). giant, H-R diagram, luminosity, main sequence, star, supergiant, white dwarf. Fill out the chart at right. Betelgeuse is rapidly recovering luminosity at an average rate of 0.02 magnitudes per day in the last week of March 2020. Betelgeuse is estimated to have surface temperatures of around 3200C (5800F), around 60% as hot as the sun. AAVSO Alert Notice 690 requests photometry and spectroscopy of alpha Ori (alf Ori, Betelgeuse) during and beyond its current minimum. An AAVSO a-scale chart is also available. According to the researchers, that can also be explained by the merger. Either scenario would lead astronomers to re-think completely current ideas of how stars evolve. Indeed, when at maximum, Betelgeuse sometimes rises to magnitude 0.4 when it becomes a fierce competitor to Rigel; in 1839 and 1852 it was thought by some observers to be nearly the equal of Capella. Dupree explains that the spot might change position over time. The M refers to the star’s colour, red, and the ‘Iab’ suffix indicates that the star is an intermediate luminosity supergiant. Hubble Space Telescope Captures First Direct Image of a Star (1995). How do the stars’ luminosity compare with their radii? Thanks for taking the data. : Naos is a star in the Argos constellation. Betelgeuse also rotates very rapidly, with a rotational velocity of about 5.5 km/second, compared to our Sun at just under 2 km/second. Recently acquiring fame for being the first star to have its atmosphere directly imaged (shown above), Alpha Orionis has captivated observers' attention for centuries.
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