Английская Википедия:GK Persei

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Шаблон:Short description Шаблон:Use dmy dates Шаблон:Starbox begin Шаблон:Starbox image Шаблон:Starbox observe Шаблон:Starbox character Шаблон:Starbox astrometry Шаблон:Starbox orbit Шаблон:Starbox detail Шаблон:Starbox catalog Шаблон:Starbox reference Шаблон:Starbox endGK Persei (also Nova Persei 1901) was a bright nova first observed on Earth in 1901. It was discovered by Thomas David Anderson, an Edinburgh clergyman, at 02:40 UT on 22 February 1901 when it was at magnitude 2.7. It reached a maximum magnitude of 0.2, the brightest nova of modern times until Nova Aquilae 1918. After fading into obscurity at about magnitude 12 to 13 during the early 20th century, GK Persei began displaying infrequent outbursts of 2 to 3 magnitudes (about 7 to 15 times quiescent brightness). Since about 1980, these outbursts have become quite regular, typically lasting about two months and occurring about every three years. Thus, GK Persei seems to have changed from a classical nova like Nova Aquilae 1918 to something resembling a typical dwarf nova-type cataclysmic variable star.

Surrounding GK Persei is the Firework nebula, a nova remnant first detected in 1902 consisting of an expanding cloud of gas and dust bubbles moving up to 1200 km/s.

Файл:GKPerLightCurve.png

The light curve of GK Persei, plotted from AAVSO data. The main plot shows the major outburst in 1901. Subplot A shows the minor outbursts which have been occurring about every 3 years since around 1980. Subplot B shows the outburst that occurred in 2018, on an expanded scale.

GK Persei has precise parallaxes reported from Gaia DR2 and Gaia EDR3, but these are thought to be badly affected by the binary nature of the system. The Hubble Space Telescope has used a different method to derive the distance to GK Persei using nebular expansion velocity and compares that with its own astrometric parallax calculation. This gave a somewhat smaller parallax (larger distance) than the Gaia measurements.

Properties

Novae consist of a main-sequence to giant star that accretes mass onto a white dwarf. The two stars of GK Persei orbit each other with a period of nearly 2 days. The white dwarf, with a mass of Шаблон:Solar mass, has one of the highest masses measured in a cataclysmic variable. The donor star, having donated much of its mass to the white dwarf, is only Шаблон:Solar mass despite being a subgiant star.

Gallery

• The location of GK Persei (circled in red)

  The location of GK Persei (circled in red)

• GK Persei by the 32-inch Schulman Telescope at the Mt. Lemmon Observatory.

  GK Persei by the 32-inch Schulman Telescope at the Mt. Lemmon Observatory.

• Expanding Nebula around GK Persei. Images range from 1953 to 2012.

  Expanding Nebula around GK Persei. Images range from 1953 to 2012.

• Changing light-echo observed at the time of the 1901 Nova, hand-drawn by G.W. Ritchey at the Yerkes Observatory. First image is from 20 September 1901. Second image (with letters a-f) is from 13 November 1901.

  Changing light-echo observed at the time of the 1901 Nova, hand-drawn by G.W. Ritchey at the Yerkes Observatory.

External links

• http://www.daviddarling.info/encyclopedia/N/Nova_Persei_1901.html
• http://lheawww.gsfc.nasa.gov/users/mukai/iphome/systems/gkper.html
• GK Persei from the AAVSO
• APOD: GK Per: Nova of 1901, 2011 November 5
• GK Persei by Chandra
• Video showing the expansion of the nova remnant