GK Persei
| Doppelstern GK Persei | |||||||||||
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| Überlagerung von Aufnahmen der Nova GK Persei im Röntgenbereich, blau, im optischen Bereich, gelb und im Radiowellen-Bereich, rosa; erstellt aus Aufnahmen des Chandra-Weltraumteleskops, des Hubble-Weltraumteleskops und des Very Large Array | |||||||||||
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| AladinLite | |||||||||||
| Beobachtungsdaten Äquinoktium: J2000.0, Epoche: J2000.0 | |||||||||||
| Sternbild | Perseus | ||||||||||
| Rektaszension | 03h 31m 12,01s [1] | ||||||||||
| Deklination | +43° 54′ 15,5″ [1] | ||||||||||
| Helligkeiten | |||||||||||
| Scheinbare Helligkeit | 14,0 mag [1] | ||||||||||
| Spektrum und Indices | |||||||||||
| Veränderlicher Sterntyp | NA/DQ+UG[2] | ||||||||||
| Spektralklasse | WD + K2 IVe [2] | ||||||||||
| Astrometrie | |||||||||||
| Radialgeschwindigkeit | (5,7 ± 2) km/s [1] | ||||||||||
| Parallaxe | (2,26 ± 0,04) mas [1] | ||||||||||
| Entfernung | (1450) Lj (440) pc | ||||||||||
| Eigenbewegung [1] | |||||||||||
| Rek.-Anteil: | (−6,71 ± 0,08) mas/a | ||||||||||
| Dekl.-Anteil: | (−17,19 ± 0,07) mas/a | ||||||||||
| Physikalische Eigenschaften | |||||||||||
| Masse | (0,87 ± 0,08 / ?) M☉ [3] | ||||||||||
| Effektive Temperatur | (5100) K [1] | ||||||||||
| Metallizität [Fe/H] | (−0,125) [1] | ||||||||||
| Andere Bezeichnungen und Katalogeinträge | |||||||||||
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GK Persei (auch Nova Persei 1901) war eine Nova, die 1901 im Sternbild Perseus aufleuchtete und mit einer maximalen Helligkeit von 0,2 mag eine der hellsten neuzeitlich beobachteten Novae war. Als Novaüberrest, mit einer Ruhehelligkeit von 13,5 mag, ist GK Persei ein kataklysmischer Veränderlicher (CV), der eine Reihe von Eigenschaften in sich vereint, die in dieser Kombination selten auftreten: Die Bahnperiode von GK Persei gehört mit 1,99 Tagen[4] zu den längsten in CVs beobachteten, und der Begleitstern ist ein Unterriese, und nicht wie in der Regel ein Hauptreihenstern. Der akkretierende Weiße Zwerg ist magnetisch und rotiert mit einer Periode von 351 Sekunden[5], womit GK Persei den asynchronen, magnetischen CVs des Typs DQ-Herculis zuzuordnen ist.
Darüber hinaus werden in GK Persei Zwergnova-Ausbrüche beobachtet, bei denen die Helligkeit des Systems um 2 bis 3 Magnituden ansteigt. Die Ausbrüche treten in Abständen von ungefähr drei Jahren auf und dauern ca. zwei Monate.
GK Persei wird von einer expandierenden Hülle umgeben, die vom letzten Novaausbruch stammt und die gelegentlich als fireworks nebula bezeichnet wird.
Rezeption
In seiner Kurzgeschichte Beyond the Wall of Sleep (deutsch: Jenseits der Mauer des Schlafes ) verarbeitete der amerikanische Schriftsteller H. P. Lovecraft die Nova Persei als Kurzgeschichte, bei der ein außerirdisches Wesen im Körper eines Menschen auf Rache an dem Stern Algol sinnt.[6]
Weblinks
- http://asd.gsfc.nasa.gov/Koji.Mukai/iphome/systems/gkper.html
- https://www.aavso.org/vsots_gkper
- http://www.daviddarling.info/encyclopedia/N/Nova_Persei_1901.html
Einzelnachweise
- ↑ a b c d e f g GK Per. In: SIMBAD. Centre de Données astronomiques de Strasbourg, abgerufen am 26. August 2018.
- ↑ a b GK Per. In: VSX. AAVSO, abgerufen am 10. Dezember 2018.
- ↑ Wada, Y. et al.: An Estimation of the White Dwarf Mass in the Dwarf Nova GK Persei with NuSTAR Observations of Two States. In: MNRAS. 474. Jahrgang, Nr. 2, Februar 2018, S. 1564–1571, doi:10.1093/mnras/stx2880, arxiv:1711.01727, bibcode:2018MNRAS.474.1564W.
- ↑ Crampton D., Fisher W.A., Cowley A.P.: The orbit of GK Persei. In: The Astrophysical Journal. 300. Jahrgang, 1986, S. 788, doi:10.1086/163856, bibcode:1986ApJ...300..788C.
- ↑ Mauche C.W.: The Spin-Up Rate of the White Dwarf in GK Per. In: ASP Conference Proceedings. 315. Jahrgang, 2004, S. 120, bibcode:2004ASPC..315..120M.
- ↑ „Beyond the Wall of Sleep.“ In: S. T. Joshi, David E. Schultz: An H.P. Lovecraft Encyclopedia. Greenwood Publishing Group, 2001; S. 19.
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Autor/Urheber: IAU and Sky & Telescope magazine (Roger Sinnott & Rick Fienberg), Lizenz: CC BY 3.0
IAU Perseus chart
"Mini Supernova" Explosion Could Have Big Impact
http://www.nasa.gov/mission_pages/chandra/mini-supernova-explosion-could-have-big-impact.html
In Hollywood blockbusters, explosions are often among the stars of the show. In space, explosions of actual stars are a focus for scientists who hope to better understand their births, lives, and deaths and how they interact with their surroundings.
Using NASA’s Chandra X-ray Observatory, astronomers have studied one particular explosion that may provide clues to the dynamics of other, much larger stellar eruptions.
A team of researchers pointed the telescope at GK Persei, an object that became a sensation in the astronomical world in 1901 when it suddenly appeared as one of the brightest stars in the sky for a few days, before gradually fading away in brightness. Today, astronomers cite GK Persei as an example of a “classical nova,” an outburst produced by a thermonuclear explosion on the surface of a white dwarf star, the dense remnant of a Sun-like star.
A nova can occur if the strong gravity of a white dwarf pulls material from its orbiting companion star. If enough material, mostly in the form of hydrogen gas, accumulates on the surface of the white dwarf, nuclear fusion reactions can occur and intensify, culminating into a cosmic-sized hydrogen bomb blast. The outer layers of the white dwarf are blown away, producing a nova outburst that can be observed for a period of months to years as the material expands into space.
Classical novas can be considered to be “miniature” versions of supernova explosions. Supernovas signal the destruction of an entire star and can be so bright that they outshine the whole galaxy where they are found. Supernovas are extremely important for cosmic ecology because they inject huge amounts of energy into the interstellar gas, and are responsible for dispersing elements such as iron, calcium and oxygen into space where they may be incorporated into future generations of stars and planets.
Although the remnants of supernovas are much more massive and energetic than classical novas, some of the fundamental physics is the same. Both involve an explosion and creation of a shock wave that travels at supersonic speeds through the surrounding gas.
The more modest energies and masses associated with classical novas means that the remnants evolve more quickly. This, plus the much higher frequency of their occurrence compared to supenovas, makes classical novas important targets for studying cosmic explosions.
Chandra first observed GK Persei in February 2000 and then again in November 2013. This 13-year baseline provides astronomers with enough time to notice important differences in the X-ray emission and its properties.
This new image of GK Persei contains X-rays from Chandra (blue), optical data from NASA’s Hubble Space Telescope (yellow), and radio data from the National Science Foundation’s Very Large Array (pink). The X-ray data show hot gas and the radio data show emission from electrons that have been accelerated to high energies by the nova shock wave. The optical data reveal clumps of material that were ejected in the explosion. The nature of the point-like source on the lower left is unknown.
Over the years that the Chandra data span, the nova debris expanded at a speed of about 700,000 miles per hour. This translates to the blast wave moving about 90 billion miles during that period.
One intriguing discovery illustrates how the study of nova remnants can provide important clues about the environment of the explosion. The X-ray luminosity of the GK Persei remnant decreased by about 40% over the 13 years between the Chandra observations, whereas the temperature of the gas in the remnant has essentially remained constant, at about one million degrees Celsius. As the shock wave expanded and heated an increasing amount of matter, the temperature behind the wave of energy should have decreased. The observed fading and constant temperature suggests that the wave of energy has swept up a negligible amount of gas in the environment around the star over the past 13 years. This suggests that the wave must currently be expanding into a region of much lower density than before, giving clues to stellar neighborhood in which GK Persei resides.
A paper describing these results appeared in the March 10th issue of The Astrophysical Journal. The authors were Dai Takei (RIKEN, Spring-8 Center Japan), Jeremy Drake (Smithsonian Astrophysical Observatory), Hiroya Yamaguichi (Goddard Space Flight Center), Patrick Slane (Smithsonian Astrophysical Observatory), Yasunobu Uchimaya (Rikkyo University, Japan), Satoru Katsuda (Japanese Aerospace Exploration Agency).
NASA's Marshall Space Flight Center in Huntsville, Alabama, manages the Chandra program for NASA's Science Mission Directorate in Washington. The Smithsonian Astrophysical Observatory in Cambridge, Massachusetts, controls Chandra's science and flight operations.