Wolf 1055 ( Latin Wolf 1055 ) is a double star in the constellation Eagle . It is located at a distance of about 19 light years from the sun . The unofficial name for component B is Van Bisbrook Star.
| Wolf 1055 AB | |||
|---|---|---|---|
| Star | |||
 | |||
| Observational data ( Age J2000.0 ) | |||
| Right ascension | |||
| Declination | |||
| Distance | 19.2 St. years old | ||
| Visible magnitude ( V ) | 9.13 | ||
| Constellation | Eagle | ||
| Astrometry | |||
| Radial velocity ( R v ) | 32.4 km / s | ||
| Own movement (μ) | RA: -578.80 mas per year Dec: -1331.57 mas per year | ||
| Parallax (π) | 170.25 mas | ||
| Absolute magnitude (V) | 10.63 | ||
| Specifications | |||
| Spectral class | M3.5 Vne / M8 Ve | ||
| Variability | flashing | ||
| physical characteristics | |||
| Weight | 48% / 9% M ☉ | ||
| Radius | 54.2% / 10.2% R ☉ | ||
| Temperature | / 2700 K | ||
| |||
| Database Information | |||
| SIMBAD | |||
Study History
The star was first registered by Maximilian Wolf in 1919 . Later, the American astronomer Frank Ross calculated his own motion of the main component of the system, Wolf 1055 A, publishing the data in May 1928 [2] . In 1940, Georges van Bisbrook discovered [3] the second component, Wolf 1055 B, which later began to bear his name. In 1944, van Bisbrook recorded the maximum distance at which both stars move away from each other - 77 “or 440 a. e. [4]
Features
Both components are rather dull, therefore they are not visible to the naked eye; both of them belong to the class of flashing stars .
Wolf 1055 A
The component Wolf 1055 A is a cold and dull red dwarf , having a mass and diameter of 48% and 54.2% of the solar, respectively; luminosity does not exceed 0.2% of the solar [5] . As a variable star, this component has the additional designation V1428 Eagle .
Wolf 1055 V (Van Bisbruck Star)
The second component is Wolf 1055 V. In size and mass, it is even inferior to the Sun. It has only about 9% of the mass, 10.2% of the diameter of the Sun, which brings it closer to the size of Jupiter [5] . The surface temperature of the star is about 2700 degrees Kelvin [6] . In 1994, a team of astronomers recorded a powerful flash on a star, its surface temperature increased 50 thousand times [5] . Researchers believe that this event is due to a powerful manifestation of the magnetic field of the star. In 2000, Wolf 1055 V recorded a powerful flash, visible in the X-ray range, which confirms the data on coronal activity [7] .
Planet System
The star Wolf 1055 A with observations from the CARMENES spectrograph and the archived data of the HIRES and HARPS spectrographs has discovered an exoplanet , called by discoverers not Wolf 1055 A b , but HD 180617 b (according to the designation of star A in the Henry Draper astronomical catalog ). The discovery was made using the radial velocity method. The minimum mass of the planet is 12.2 + 1.0 / -1.4 Earth masses (comparable to the mass of Neptune ), the circulation period is 105.9 ± 0.1 days, the eccentricity is 0.16 + 0.05 / -0, 10, semi-major axis - 0.3357 AU The orbit HD 180617 b passes near the far boundary of the habitat zone of the star Wolf 1055 A [8] [9] .
Nearest star environment
The closest star to the Wolf 1055 AB system is Altair . In the night sky of hypothetical planets revolving around the components of Wolf 1055, Altair, having an absolute magnitude of 2.22 m , from a distance of 3.7 sv. years (1.13 pc) will have a visible magnitude of -2.515 m .
The following star systems are within 10 light-years of Wolf 1055:
| Star | Spectral class | Distance, st. years old |
| Altair | A7 v | 3,7 |
| 70 Ophiuchus AB | K0 Ve / K5 Ve | 6.1 |
| G 184-19 AB | M4.5 V / M4.5 V | 9.3 |
| ISO 417 | M1 V | 9.7 |
| BD-03 4233 | M0 V | 9.9 |
Notes
- ↑ 1 2 3 4 Gaia Data Release 2 - 2018.
- ↑ Ross, FE New proper-motion stars, (sixth list ) . Astronomical Journal, vol. 38, iss. 900, p. 117-120 (1928). (May 15, 1928). Date of treatment March 19, 2009. Archived March 28, 2012.
- ↑ van Biesbroeck, G. The star of lowest known luminosity. (eng.) . Astronomical Journal, Vol. 51, p. 61. (1944). Date of treatment March 19, 2009. Archived March 28, 2012.
- ↑ van Biesbroeck, G. A search for Stars of Low Luminosity. (eng.) . Astron. J. 66, 528-530 (1961) (July 13, 1961). Date of treatment March 19, 2009. Archived March 28, 2012.
- ↑ 1 2 3 JL Linsky, BE Wood, A. Brown, MS Giampapa, C. Ambruster. Stellar Activity at the End of the Main Sequence: GHRS Observations of the M8 Ve Star VB 10. (English) (PDF). Astron. J., 455: 570-676 (1995) (March 1, 1995). Date of treatment March 19, 2009. Archived March 28, 2012.
- ↑ Schweitzer, A., Hauschildt, PH, & Allard, F. Pressure broadening in M dwarfs and VB 10. (English) (PDF). Cool stars stellar systems; and the sun: 9: Astronomical Society of the Pacific Conference Series, volume 109 (1996). Date of treatment March 19, 2009. Archived March 28, 2012.
- ↑ Fleming, Thomas A .; Giampapa, Mark S .; Schmitt, Jürgen HMM An X-Ray Flare Detected on the M8 Dwarf VB 10. (Eng.) . The Astrophysical Journal, Volume 533, Issue 1, pp. 372-377. (04/2000). Date of treatment March 19, 2009. Archived March 28, 2012.
- ↑ The CARMENES search for exoplanets around M dwarfs
- ↑ Exoplanet found in the “zone of life” of a close binary system , 09/02/2018
See also
- Eagle constellation star list