{"id":7972,"date":"2023-08-14T16:28:23","date_gmt":"2023-08-14T16:28:23","guid":{"rendered":"https:\/\/power2innovate.com\/a-jupiter-hotter-than-the-sun\/"},"modified":"2023-08-14T16:28:23","modified_gmt":"2023-08-14T16:28:23","slug":"a-jupiter-hotter-than-the-sun","status":"publish","type":"post","link":"https:\/\/power2innovate.com\/a-jupiter-hotter-than-the-sun\/","title":{"rendered":"A ‘Jupiter’ hotter than the sun"},"content":{"rendered":"
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\n\n \n Phased radial-velocity curves of WD 0032\u2013317. a<\/b>, Trailed UVES spectrum for the H\u03b1<\/i> line of WD 0032\u2013317 (blue represents lower fluxes and yellow represents higher fluxes), folded over the orbital period (P<\/i>\u2009=\u20098340.9090\u2009s). The primary absorption is clearly seen in blue. The emission from the companion (in yellow) appears in antiphase with the primary and is visible only from the irradiated day side, between orbital phases ~0.2\u20130.8. Its \u2018inverted\u2019 shape, evident especially near quadrature, is the result of NLTE effects58<\/sup>. b<\/b>, Radial-velocity curves (top panel) of the white dwarf (blue circles) and the irradiated companion (red diamonds), folded over the orbital period (P<\/i>\u2009=\u20098340.9090\u2009s). The primary\u2019s (secondary\u2019s) best-fit curve is marked by the blue dashed (red dotted) line on both panels. The bottom panels show the residuals of the white dwarf component (middle) and the irradiated companion (bottom). The error bars show the standard deviation. The illustrations on the top of b<\/b> demonstrate the system\u2019s configuration at each orbital phase. Credit: Nature Astronomy<\/i> (2023). DOI: 10.1038\/s41550-023-02048-z \n <\/figcaption><\/figure>\n<\/p><\/div>\n<\/div>\n
The search for exoplanets\u2014planets that orbit stars located beyond the borders of our solar system\u2014is a hot topic in astrophysics. Of the various types of exoplanets, one is hot in the literal sense: hot Jupiters, a class of exoplanets that are physically similar to the gas giant planet Jupiter from our own neighborhood.<\/p>\n\n <\/p>\n<\/section>\n
Unlike “our” Jupiter, hot Jupiters orbit very close to their stars, complete a full orbit in just a few days or even hours, and\u2014as their name suggests\u2014have extremely high surface temperatures. They hold great fascination for the astrophysics community. However, they are difficult to study because the glare from the nearby star makes them hard to detect.\n<\/p>\n
Now, in a study published today in Nature Astronomy<\/i>, scientists report the discovery of a system consisting of two celestial bodies, located about 1,400 light years away, that, together, offer an excellent opportunity for studying hot Jupiter atmospheres, as well as for advancing our understanding of planetary and stellar evolution.\n<\/p>\n
The discovery of this binary system\u2014the most extreme of its kind known so far in terms of temperature\u2014was made through analysis of spectroscopic data gathered by the European Southern Observatory’s Very Large Telescope in Chile.\n<\/p>\n
“We’ve identified a star-orbiting hot Jupiter-like object that is the hottest ever found, about 2,000 degrees hotter than the surface of the sun,” says lead author of the study Dr. Na’ama Hallakoun, a postdoctoral fellow associated with Dr. Sagi Ben-Ami’s team in the Particle Physics and Astrophysics Department at the Weizmann Institute of Science.\n<\/p>\n
She adds that, unlike glare-obscured hot-Jupiter planets, it is possible to see and study this object because it is very large compared to the host star it orbits, which is 10,000 times fainter than a normal star. “This makes it a perfect laboratory for future studies of hot Jupiters’ extreme conditions,” she says.\n<\/p>\n
An extension of research she conducted in 2017 with Prof. Dan Maoz, her Ph.D. advisor at Tel Aviv University, Hallakoun’s new discovery may make it possible to gain a clearer understanding of hot Jupiters, as well as of the evolution of stars in binary systems.<\/p>\n
Massive brown dwarf with a ‘Moon-like’ orientation<\/h2>\n
The binary system that Hallakoun and colleagues discovered involves two celestial objects that are both called “dwarfs,” but that are very different in nature. One is a “white dwarf,” the remnant of a sun-like star after it has depleted its nuclear fuel. The other part of the pair, not a planet or a star, is a “brown dwarf”\u2014a member of a class of objects that have a mass between that of a gas giant like Jupiter and a small star.\n<\/p>\n
Brown dwarfs are sometimes called failed stars because they are not massive enough to power hydrogen fusion reactions. However, unlike gas giant planets, brown dwarfs are massive enough to survive the “pull” of their stellar partners.\n<\/p>\n
“Stars’ gravity can cause objects that get too close to break apart, but this brown dwarf is dense, with 80 times the mass of Jupiter squeezed into the size of Jupiter,” Hallakoun says. “This allows it to survive intact and form a stable, binary system.”\n<\/p>\n
When a planet orbits very close to its star, the differential forces of gravity acting on the near and far side of the planet can cause the planet’s orbital and rotational periods to become synchronized. This phenomenon, called “tidal locking,” permanently locks one side of the planet in a position that faces the star, similarly to how Earth’s moon always faces Earth, while its so-called “dark side” remains out of sight. Tidal locking leads to extreme temperature differences between the “dayside” hemisphere bombarded by direct stellar radiation and the other, outward-facing “nightside” hemisphere, which receives a much smaller amount of radiation.\n<\/p>\n
The intense radiation from their stars causes hot Jupiters’ extremely high surface temperatures, and the calculations Hallakoun and her colleagues made about the paired white dwarf-brown dwarf system show just how hot things can get. Analyzing the brightness of the light emitted by the system, they were able to determine the orbiting brown dwarf’s surface temperature in both hemispheres.\n<\/p>\n
The dayside, they discovered, has a temperature of between 7,250 and 9,800 Kelvin (about 7,000 and 9,500 Celsius), which is as hot as an A-type star\u2014Sun-like stars that can be twice as massive as the Sun\u2014and hotter than any known giant planet. The temperature of the nightside, on the other hand, is between 1,300 and 3,000 Kelvin (about 1,000 and 2,700 Celsius), resulting in an extreme temperature difference of about 6,000 degrees between the two hemispheres.\n<\/p>\n
A rare glimpse into an unexplored region<\/h2>\n
Hallakoun says that the system she and her colleagues discovered offers an opportunity to study the effect of extreme ultraviolet radiation on planetary atmospheres. Such radiation plays an important role in a variety of astrophysical environments, from star-forming regions, through primordial gas disks from which planets are formed around stars, to the atmospheres of planets themselves. This intense radiation, which can lead to gas evaporation and the breaking of molecules, can have a significant impact on both stellar and planetary evolution. But that’s not all.\n<\/p>\n
“Merely one million years since the formation of the white dwarf in this system\u2014a minuscule amount of a time on the astronomical scale\u2014we have gotten a rare glimpse into the early days of this kind of compact binary system,” Hallakoun says. She adds that, while the evolution of single stars is fairly well known, the evolution of interacting binary systems is still poorly understood.\n<\/p>\n
“Hot Jupiters are the antithesis of habitable planets\u2014they are dramatically inhospitable places for life,” Hallakoun says. “Future high-resolution spectroscopic observations of this hot Jupiter-like system\u2014ideally made with NASA’s new James Webb Space Telescope\u2014may reveal how hot, highly irradiated conditions impact atmospheric structure, something that could help us understand exoplanets elsewhere in the universe.”<\/p>\n
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More information:<\/strong> \n\t\t\t\t\t\t\t\t\t\t\t\tNa’ama Hallakoun, An irradiated-Jupiter analogue hotter than the Sun, Nature Astronomy<\/i> (2023). DOI: 10.1038\/s41550-023-02048-z www.nature.com\/articles\/s41550-023-02048-z<\/p>\n<\/p><\/div>\n
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\n\t\t\t\t\t\t\t\t\t\t\t\t\tProvided by \n\t\t\t\t\t\t\t\t\t\t\t\t\t\t\t\t\t\t\t\t\t\t\t\t\t\t\tWeizmann Institute of Science<\/p>\n