Fail:A cosmic couple.jpg

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Klõps ikoonil viib faili leheküljele Wikimedia Commonsis.
Allikas: Vikipeedia

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See fail ja sellest kastist allapoole jääv kirjeldus pärinevad kesksest failivaramust Wikimedia Commons. Faili lehekülg Commonsis Faili lehekülg Commonsis

Lühikirjeldus

Kirjeldus
English: Here we see the spectacular cosmic pairing of the star Hen 2-427 — more commonly known as WR 124 — and the nebula M1-67 which surrounds it. Both objects, captured here by the NASA/ESA Hubble Space Telescope are found in the constellation of Sagittarius and lie 15 000 light-years away.

The star Hen 2-427 shines brightly at the very centre of this explosive image and around the hot clumps of gas that are ejected into space at over 150 000 kilometres per hour.

Hen 2-427 is a Wolf–Rayet star, named after the astronomers Charles Wolf and Georges Rayet. Wolf–Rayet are super-hot stars characterised by a fierce ejection of mass.

The nebula M1-67 is estimated to be no more than 10 000 years old — just a baby in astronomical terms — but what a beautiful and magnificent sight it makes.

A version of this image was released in 1998, but has now been re-reduced with the latest software.
Kuupäev (released)
Allikas http://www.spacetelescope.org/images/potw1533a/
Autor ESA/Hubble & NASA; Acknowledgement: Judy Schmidt (geckzilla.com)
Teised versioonid https://www.flickr.com/photos/gsfc/20140593234/

Litsents

w:et:Creative Commons
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 ESA/Hubble images, videos and web texts are released by the ESA under the Creative Commons Attribution 4.0 International license and may on a non-exclusive basis be reproduced without fee provided they are clearly and visibly credited. Detailed conditions are below; see the ESA copyright statement for full information. For images created by NASA or on the hubblesite.org website, or for ESA/Hubble images on the esahubble.org site before 2009, use the {{PD-Hubble}} tag.
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w:et:Creative Commons
omistamine
See fail kuulub Creative Commonsi rahvusvahelise litsentsi "Autorile viitamine 4.0" alla.
Omistamine: ESA/Hubble
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