Mu Hercules ( Latin Mu Herculis ) is a multiple system consisting of three, or possibly four stars, which is located in the constellation Hercules at a distance of about 27.4 light-years from us.
| μ Hercules | |||
|---|---|---|---|
| Multiple star | |||
| Observational data ( Age J2000.0 ) | |||
| Right ascension | |||
| Declination | |||
| Distance | 27.4 St. years old | ||
| Visible magnitude ( V ) | |||
| Constellation | Hercules | ||
| Astrometry | |||
| Radial velocity ( R v ) | |||
| Own movement (μ) | RA: -13.8 mas per year Dec: 16.5 mas per year | ||
| Absolute magnitude (V) | |||
| Specifications | |||
| Spectral class | |||
| physical characteristics | |||
| Metallicity | |||
| |||
| Database Information | |||
| SIMBAD | data | ||
| The star has 4 components Their parameters are presented below: | |||
| Sources: [2] | |||
Content
Features
The Hercules μ system consists of three components, the main of which, component A, revolves around a common center of mass along with a pair of B and C. The distance between component A and a pair of aircraft is about 286 a. e. (34.0 "). In turn, components B and C are separated by an average distance of 11.4 a. e. Since their orbit is elliptical (e = 0.18), this figure fluctuates between 9.4 and 13.5 AU. Stars B and C complete a complete revolution around the common center of mass in 43.2 years.
μ Hercules A
The main component is a yellow subgiant with a mass almost equal to the mass of the Sun. [5] Its diameter is estimated at 1.77-1.86, and the luminosity at 2.2-2.7 solar. Using a SARG spectrograph with an Echelle lattice , a group of Italian astronomers found the star’s oscillations in the spectrum, almost identical to solar. [6] Around the component A, perhaps, a massive stellar or substellar object is drawn.
μ Hercules B
Component B belongs to the class of red dwarfs of the main sequence . Its mass and diameter are approximately equal to 31% and 48% of the solar, respectively. [7] It is an extremely dim star with a luminosity equivalent to 5/1000 solar luminosity. The habitable zone , that is, the zone suitable for earth-like planets with liquid water, near it will be within 0.5 a. e. with an orbital period of 8 days.
μ Hercules C
The third star in the system is a dull and relatively cold red dwarf, similar in its characteristics to component B. The mass and diameter of the star are 31% and 25% solar, respectively. [7]
μ Hercules D?
Astrometric analysis of the data indicates the possible presence of a fourth massive object in the μ Hercules system. [8] According to some researchers, this should be a star with a mass of 1.2 solar masses, which revolves around the main component A at a distance of 17.2 a. e. and whose orbital period should be 65 years. According to others, it should be a brown dwarf , or even a supermassive Jupiter-like planet , [9] however, no clear evidence has yet been found in favor of this or that hypothesis.
Nearest star environment
μ Hercules belongs to the moving group of stars Wolf 630 - one of the largest groups located in our Galaxy . [10] The following stellar systems are within 10 light-years of the Hercules μ system:
| Star | Spectral class | Distance, st. years old |
| BD + 18 3421 | M0 V | 4,5 |
| G 184-19 | M4.5 V / M4.5 V | 6.5 |
| Vega | A0 v | 7.3 |
| BD + 25 3173 | M2 V | 8.5 |
| BD + 33 2777 | K7 V | 8.6 |
| G 203-47 | M3.5 V | 8.6 |
| BD + 43 2796 | M3.5 V | 8.7 |
| G 169-29 | MV | 8.9 |
| AC + 20 1463-148 A | M2 V-VI | 9.6 |
| AC + 20 1463-148 B | M2 V-VI | 9.8 |
See also
- List of stars of the constellation Hercules
Notes
- ↑ 1 2 3 4 5 C. Soubiran Vertical distribution of Galactic disk stars // Astron. Astrophys. - EDP Sciences , 2008. - Vol. 480, Iss. 1. - P. 91–101. - ISSN 0004-6361 ; 0365-0138 ; 1432-0746 ; 1286-4846 - doi: 10.1051 / 0004-6361: 20078788 - arXiv: 0712.1370
- ↑ SIMBAD . - μ Hercules in the SIMBAD database . Date of appeal October 15, 2009.
- ↑ SIMBAD Astronomical Database
- ↑ SIMBAD Astronomical Database
- ↑ Bedding, TR, Kjeldsen, H., Reetz, J., & Barbuy, B. Measuring stellar oscillations using equivalent widths of absorption lines . Monthly Notices of the Royal Astronomical Society, Volume 280, Issue 4, pp. 1155-1161. (1996). Date of treatment October 20, 2009. Archived April 9, 2012.
- ↑ A. Bonanno, S. Benatti, R. Claudi, S. Desidera, R. Gratton, S. Leccia, L. Patno. Detection of solar-like oscillations in the G5 subgiant mu-Herculis . Arxiv.org (Jan 29, 2008). Date of treatment October 20, 2009.
- ↑ 1 2 Wanner, JF Masses of the Dwarf M Stars in the MU Herculis System. (eng.) . Astronomical Journal, Vol. 72, p. 836 (1967). Date of treatment October 20, 2009. Archived April 9, 2012.
- ↑ Heintz, WD Photographic astrometry of binar and proper-motion stars: 8. (Eng.) . Astronomical Journal (ISSN 0004-6256), vol. 108, no. 6, p. 2338-2347 (1994). Date of treatment October 20, 2009. Archived April 9, 2012.
- ↑ Cochran, William D .; Hatzes, Artie P. A high-precision radial-velocity survey for other planetary systems . Astrophysics and Space Science, vol. 212, nos. 1-2, p. 281-291 (02/1994). Date of treatment October 20, 2009. Archived April 9, 2012.
- ↑ McDonald, ARE & Hearnshaw, JB The Wolf 630 moving group of stars . Royal Astronomical Society, Monthly Notices (ISSN 0035-8711), vol. 204, Aug. 1983, p. 841-852. (Aug. 1983). Date of treatment October 20, 2009. Archived April 9, 2012.