An international team of astronomers has observed an infrared dark cloud surrounding a baby star that is about ten times larger than those found around typical solar-mass baby stars.
A baby star is surrounded by the natal gas and dust cloud, and the cloud is warmed up from its center.
The team also observed radio emission from carbon sulfide (CS) and silicon monoxide (SiO) to reveal the detailed structure of the molecular outflow from the baby star. However you pronounce its name*, the star Betelgeuse is hard to miss on a clear winter's night. The ejected outer layers of the star expanded outwards until they hit the surrounding material, creating the arc-like structures seen to the left of the image. Further to the left is what appears to be a straight wall of gas and dust, the origin of which is uncertain. It may be material that was shed by Betelgeuse at an earlier stage - and so has had longer to travel outwards - but it is then hard to explain why it is so straight.
Another possibility is that it is just a part of the cloud that Betelgeuse is moving through, and which is being illuminated by the star's own starlight. The immediate surroundings of Betelgeuse look much brighter than the regions further out, implying that around 30,000 years ago the star starting shedding mass at a higher rate. While many exoplanets have been discovered and confirmed over the past couple of decades using various techniques, very few have actually been directly imaged. The left image shows shows normal light, including both the dust ring and the residual light from the central star scattered by turbulence in Earth’s atmosphere. GPI’s success in imaging previously-known systems like Beta Pictoris and HR4796A can only indicate many more exciting exoplanet discoveries to come. This year the GPI team will begin a large-scale survey, looking at 600 young stars to see what giant planets may be orbiting them. A graphic designer in Rhode Island, Jason writes about space exploration on his blog Lights In The Dark, Discovery News, and, of course, here on Universe Today. We’ll be releasing data to the community in mid February via the Gemini Observatory web site.
This hot cloud is about ten times larger than those found around typical solar-mass baby stars, which indicates that the star formation process has more diversity than ever thought. Infrared Dark Clouds (IRDC) are dense regions of such clouds, and thought that in which clusters of stars are formed.

Temperature of the central part of some, but not all, of such clouds reaches as high as -160 degrees Celsius. In order to warm up the large volume of gas, the baby star should emit much more energy than typical ones. As it has swelled in size over the past few hundred thousand years, currently measuring around 1000 times the size of our Sun, the massive star has been shedding its outer layers. It is very hard to measure distances in images such as this, so the wall could be much futher away or closer to Earth than Betelgeuse - essentially in the foreground or background. It appears to be made of gas and dust of the same composition as the arcs around Betelgeuse, but is slightly cooler, at around -210 Celsius. If that is the case, and it really is in Betelgeuse's path, then in around 5000 years the arcs around Betelgeuse will plough into it, and in around 20,000 years the star itself will follow. The structure in this "inner envelope" around the star is also assymetric, suggesting that the material has not been flowing out from the star in a uniform way.
It weighs in at between 10 and 20 times the mass of our Sun, and such massive stars live fast and die young. In the meantime, Betelgeuse is providing astronomers with the opportunity to study an aging, massive star in great detail.
The name Betelgeuse literally means "armpit of the giant" in Arabic, though this is largely due to a historical mis-translation - its original name meant "shoulder of the great one, which is somewhat more dignified! Direct images of exoplanets will change public perception of the subject and probably theories of planetary formation too. I also hope they attempt to image some local systems, like Epsilon Eridani or Alpha Centauri. We may at some point be able to image Asteroid belt- and Kuiper belt-like objects around other stars, or confirm the existence of Oort cloud-like objects. Since most of stars are born as members of star clusters, investigating IRDCs has a crucial role in comprehensive understanding the star formation process.
A detailed investigation tells them that the temperature of the methanol gas is -140 degrees Celsius.
Protostars produce emission by converting the gravitational energy of infalling material to the thermal energy. At over 600 light years away Betelgeuse is not particularly close, but it shines 100,000 times as brightly as our Sun.

This material is made of gas and dust, which has cooled over time and is seen here in far-infrared light by Herschel.
But don't worry for the star - the gas clouds are incredibly thin, so such a collision would have no impact Betelgeuse itself. Betelgeuse is only around 10 million years old - a tiny fraction of the Sun's 5 billion years - but is very much in the twilight of its life. I expect it is it too late to include one in the James Webb telescope, hopefully the Chinese will put one on the moon. I hope they will image the same planet multiple times and show us a GIF of an exoplanet orbiting its star! I do believe the universe is at least as old as we’ve observed it to be, if not older due to the cosmic horizon effect. Inside hot cores, various molecules, originally trapped in the ice mantle around dust particles, are sublimated. Although molecular outflows are common features around protostars, the outflow as young as the one in MM3 is quite rare.
The large size of the hot core in MM3 is possibly due to the high mass infalling rate than ever thought. At some point in the next million years or so (a blink of an eye in astronomical terms!) the core of the star will run out of fuel, at which point Betelgeuse will die in one of the most violent events in nature - a supernova. The light from the back edge of the disk (to the right of the star) is strongly polarized as it reflects towards Earth, and thus it appears brighter than the forward-facing edge.
Not that many years ago, the most powerful telescopes couldn’t even resolve the disk of a star, let alone see a planet around one. The size of the hot core is as large as 800 times 300 astronomical units (au, 1 au equals to the mean distance of the Sun and the Earth; 150 million km). Typical size of hot cores around low-mass young stars is several tens to hundred of au, therefore the hot core in MM3 is exceptionally large.
Sakai says “Thanks to the high sensitivity and spatial resolution, we need only a few hours to discover a previously unknown baby star.

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