Last Wednesday a white-dwarf star erupted in the constellation Delphinus, producing the brightest nova since 2007. Currently shining at magnitude 4.9, the nova is visible to the unaided eye from dark locations far from city lights, and might remain so for weeks to come.
“The nova is easy to locate north of the lovely star pattern of Delphinus. And the constellation Sagitta, the Arrow, points right toward it,” says Tony Flanders, associate editor of Sky & Telescope and host of S&T’s PBS TV show SkyWeek.
“A second advantage is the nova’s location. It’s easily visible in the eastern sky in the early evening, so it can be followed for many hours. This means that amateur skygazers and professional scientists alike can continue monitoring it for months to come,” adds Arne Henden, director of the American Association of Variable Star Observers (AAVSO). “The nova can be seen with binoculars even from light-polluted metropolitan areas. Hundreds of observers, many for the first time, have submitted brightness estimates of the nova to the AAVSO.”
Nova Delphini 2013 was discovered by Koichi Itagaki of Yamagata, Japan, in an image taken at 14 hours Universal Time (2 p.m. EDT) on August 14th. It was not present in a photo that he took the previous day. The star was apparently 17th magnitude before erupting, so it brightened roughly 100,000-fold to its peak of magnitude 4.5 on August 16th. The nova declined slightly after that, but has held remarkably steady at magnitude 4.9 for the past three days.
“As for what it will do in the days ahead, your guess is as good as mine! It could remain at this brightness for many more days, it could rebrighten, or it could fade rapidly. That is what’s fun about novae,” says Henden.
A classical nova occurs in a special kind of tightly orbiting binary star system: one where a relatively normal star pours a stream of hydrogen onto the surface of a companion white dwarf. When the layer of fresh hydrogen on the white dwarf’s surface grows thick and dense enough, the bottom of the layer explodes in a runaway hydrogen-fusion reaction — a hydrogen bomb in the shape of a thin shell roughly the size of Earth. The underlying white dwarf remains intact, and as new hydrogen builds up, the process may repeat in a few years to tens of thousands of years.
“Nova Delphini 2013 is among the 30 brightest novae ever recorded,” says S&T editor in chief Robert Naeye. “It’s a wonderful target for backyard observers, given that it’s visible to the unaided eye and relatively easy to find. But it’s also attracting the intense interest of scientists, who are using a wide assortment of telescopes and astronomical satellites to better understand these enigmatic explosions.”
Novae are distant cousins to Type Ia supernovae. In novae, the surface of the white dwarf produces a powerful explosion, but the white dwarf itself survives. In a Type Ia supernovae, the white dwarf accumulates just enough mass from its binary partner to be pushed above the Chandrasekhar limit of about 1.4 solar masses. This triggers a massive thermonuclear explosion that blows the entire white dwarf to smithereens.
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