Credit & Copyright: X-ray Image:
M. Karovska
(Harvard-Smithsonian CfA)
et al.,
CXC /
NASA
Illustration: M.Weiss(CXC)
Explanation:
To seventeenth century astronomers,
Omicron
Ceti or
Mira was
known as a wonderful star - a star whose brightness could change
dramatically in the course of about 11 months.
Modern astronomers now recognize an entire class of long period
Mira-type variables as cool,
pulsating, red giant stars, 700 or so times the diameter of the Sun.
Only 420 light-years away,
red
giant Mira (Mira A, right) itself
co-orbits with a companion star, a small white dwarf (Mira B).
Mira B is surrounded by a disk of material drawn from the pulsating
giant and in such a double star system, the white dwarf star's
hot accretion disk
is expected to produce
some x-rays.
But this sharp,
false-color image from the Chandra Observatory also
captures the cool giant star strongly
flaring at
x-ray energies, clearly
separated from the x-ray emission of its companion's accretion disk.
Placing your cursor over the Chandra x-ray image of Mira will reveal
an artist's vision of this still wonderful
interacting binary star system.
Illustration: M.Weiss(CXC)
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Publikacii s klyuchevymi slovami:
binary star - variable star - accretion disk - red giant - white dwarf - Tesnye dvoinye sistemy - Peremennye zvezdy - fizicheskie dvoinye zvezdy - dvoinye sistemy - Mira
Publikacii so slovami: binary star - variable star - accretion disk - red giant - white dwarf - Tesnye dvoinye sistemy - Peremennye zvezdy - fizicheskie dvoinye zvezdy - dvoinye sistemy - Mira | |
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