Nova Persei 2018
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Double star Nova Persei 2018 |
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| Nova Persei 2018 | |||||
| AladinLite | |||||
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Observation dates equinox : J2000.0 , epoch : J2000.0 |
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| Constellation | Perseus | ||||
| Right ascension | 04 h 43 m 21.37 s | ||||
| declination | + 47 ° 21 ′ 25.9 ″ | ||||
| Apparent brightness | 16.9 mag | ||||
| Typing | |||||
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rel. Brightness (G-band) |
(16.168 ± 0.023) mag | ||||
| rel. Brightness (J-band) |
(13.77 ± 0.03) mag | ||||
| B − V color index | −1.9 | ||||
| Variable star type | NA + UG | ||||
| Astrometry | |||||
| parallax | (0.257 ± 0.052) mas | ||||
| distance | 13,000 ly 4,000 pc |
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| Proper movement | |||||
| Rec. Share: | (0.19 ± 0.10) mas / a | ||||
| Dec. portion: | (−1.75 ± 0.08) mas / a | ||||
| Physical Properties | |||||
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Other names and catalog entries |
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The Nova Persei 2018 was a bright nova that was discovered on April 29, 2018 in the constellation Perseus . Previously, it had been reported on February 16, 1970 as Zwergnova V392 Per by Gerold Alfred Richter from Sonneberg.
Dwarf Nova
A U Geminorum- type dwarf nova is a type of cataclysmic variable system that consists of a narrow binary star system in which one of the components is a white dwarf that accretes matter from a cooler star or a subgiant of the main sequence . V392 Persei was discovered in 1970 and classified as a dwarf nova, it usually has a visual strength of 17.4 mag with bursts of 2-3 orders of magnitude. The spectrum was examined in the resting state, whereby only the cool companion star was recorded. The spectrum shows emission lines of hydrogen alpha (Hα) and both neutral and ionized helium. The brightest recorded observations are at magnitude 5.6.
Nova outbreak
On April 29, 2018 it was discovered by Yuji Nakamura due to its extreme brightness and spectroscopically confirmed on April 30 as a nova outbreak with a strength of 6.2 mag. The spectrum includes broad Hα and Fe (II) emission lines with P-Cygni profiles . The middle part of the absorption spectrum has a blue shift of 2,680 km / s, which should correspond to the expansion speed of the nova explosion.
Observations with the Fermi Gamma-ray Space Telescope on April 30th show a strong gamma-ray source at the coordinates of the Nova. The photometry of the Nova from the Konkoly Observatory on May 1, 2018 showed values of 7.38 mag in the V-band and 8.22 mag in the B-band, which indicated that it had already exceeded the maximum.
system
V392 Persei is the southern component of a pair of stars that are 8.5 arc seconds apart. The symbiotic couple could not be resolved and the exact determination of the cool companion is unclear. The spectral energy distribution does not match that of a bright giant star, but it could be a group of less luminous red giants or sub-giants. If the cool component is a red dwarf from the main sequence, as would be the case with a dwarf nova, the system should be closer than the suggested 13,000 ly.
Web links
Individual evidence
- ↑ a b c d e f V392 Per. In: SIMBAD . Center de Données astronomiques de Strasbourg , accessed on March 28, 2019 .
- ↑ a b V0392 Per. In: VSX. AAVSO , accessed March 28, 2019 .
- ↑ V392 Persei - a nova with previous observations. Thorsten Lange, May 2018, accessed on March 28, 2019 .
- ^ GCVS Variability Types and Distribution Statistics of Designated Variable Stars According to their Types of Variability . February 12, 2009. Retrieved March 24, 2019.
- ↑ Optical Spectroscopy of TCP J04432130 + 4721280 (V392 Per) Confirms a Nova Eruption . Retrieved March 24, 2019.
- ↑ Bright gamma-ray emission from TCP J04432130 + 4721280 (V392 Per) detected by Fermi-LAT . Retrieved March 24, 2019.
- ↑ Optical Photometry of the Nova Outburst TCP J04432130 + 4721280 (V392 Per) . Retrieved March 24, 2019.