h Orionis
| catalogues and names | h Ori, eta Ori, 28 Ori, HR 1788, HD 35411, SAO 132071, WDS 05245-0224A |
| constellation | Orion |
data from The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version) (Hoffleit+, 1991)
position, motion, parallax:
| position (J2000) | RA: 5h 24min 28,6sec | DEC: -2° 23' 49'' |
| position (J1900) | RA: 5h 19min 26,9sec | DEC: -2° 29' 21'' |
| proper motion (J2000) | RA: 0,002 arcsec/a | DEC: 0 arcsec/a |
| radial velocity | 20 km/s note: spectroscopic binaries, double lined spectra note: orbital data avaible |
|
| rotational velocity | 46 km/s (uncertain) (variable) | |
| trigonometric parallax | 0,007 arcsec | |
| note (category: radial and/or rotational velocities): | Expanding circumstellar shell. |
| note (category: dynamical parallaxes): | 0.005". |
magnitude
| visual magnitude | 3,36 (V on UBV Johnson system) |
spectral / color information
| spectral class | B1V+B2e |
| B-V-magnitude | -0,17 |
| U-B-magnitude | -0,92 |
| R-I-magnitude | -0,23 |
variability information
| variable star identification | Eta Ori |
| note (category: variability): | EA + Beta C 3.31 - 3.60V, 3.14 - 3.35B, 7.989268d. Also sinusoidal pulsation period, amp. 0.05V, 0.30197 or 0.30145d. |
double/multiple star system information
| number of components of multiple star system | 5 |
| separation | 1,5 arcsec |
| mag difference (of double or brightest multiple) | 1,4 |
| component ID | AB |
| note (category: double and multiple data): | ADS 4002A is SB triple system, abc with periods 9.2y and 7.989d. Speckle interferometry gives 9.219y, a = 0.036" for for ab x c. Visual components AB, binary, 3.8, 4.8v, sep. 1.650"; C, 9.4v at 115". The total mass of the quintuple system exceeds 50 solar masses, the most massive component being about 17 solar masses. |
| note (category: spectroscopic binaries): | ab, 7.9841d, K 145.2k/s, V0 +35.9k/s, asini 15.9. abc, 9.2y, K 17.5k/s, V0 +19.5k/s, asini 805. Resolved by speckle interferometry at 4-meter Mayall telescope, sep. 0.04"; vsini secondary 39k/s. |
miscellaneous information
| note (category: group membership): | Ori OB1a; Orion belt; cluster CR 70. |
data from SKY2000 - Master Star Catalog (Myers+ 1997)
position, motion, parallax:
| position (J2000) | RA: 5h 24min 28,633sec | DEC: -2° 23' 49,38'' | ±0,43 arcsec | source: 16 |
| proper motion (J2000) | RA: 0,0001 arcsec/a | DEC: 0,001 arcsec/a | source: 25 | |
| radial velocity | 20 km/s | source: 25 | ||
| trigonometric parallax | 0,007 | ±0,001 arcsec | source: 25 | |
| galactic coord. (B1950) | longitude: 204,87° | latitude: -20,39° | ||
| GCI unit vector (J2000) | X: 0,154242 | Y: 0,987147 | Z: -0,041824 | |
magnitude:
| visual | 3,3 (observed) | source: 31 |
| photovisual | 3,4 | source: 2 |
| photographic | 3,2 | source: 2 |
spectral information:
| spectral class | B1 | source: 96 | |
| Morgan-Keenan | B1V+B2e | source: 25 | |
| B-magnitude | 3,19 ±0,05 | B-V-magnitude | -0,17 |
| U-magnitude | 2,27 ±0,05 | U-B-magnitude | -0,92 |
variability information:
| variability type | 10 |
| var. amplitude | 0,29 |
| var. period | 7,99 |
| var. epoch | 2415762 12. January 1902, 12:00:00 UT |
| next max light | 2451629,11 25. March 2000, 14:38:24 UT |
double/multiple star system information:
| separation between brightest and second brightest component | 1,7 arcsec |
| magnitude difference between brightest and second brightest component | 1 |
| position angle | 78 ° |
sources:
| 2 | HD and HDE Catalogs |
| Cannon, A.J., and E.C. Pickering, Harvard Annals, Vols 91-99, 1918-24, Cambridge, Massachusetts: Harvard University; Cannon, A.J., Harvard Annals, Vol. 100, 1925-36, Cambridge, Massachusetts: Harvard University; and Cannon, A.J., and M. Walton Mayall, Harvard Annals, Vol. 112, 1949, Cambridge, Massachusetts: Harvard University | |
| 16 | PPM North and PPM South Catalogs and PPM Supplement |
| Roser, S., and U. Bastian, "Catalogue of Positions and Proper Motions," A&AS, Vol. 74, p. 449, 1988, and Bastian, U., et al., "Catalogue of Positions and Proper Motions - South," 1993 | |
| 19 | WDS Catalog |
| Worley, C.E., and G.G. Douglass, Washington Catalog of Visual Double Stars 1996.0, United States Naval Observatory, 1996 | |
| 25 | Bright Star Catalogue, 5th edition |
| Hoffleit, D. and Warren, W.H. Jr., The Bright Star Catalogue, 5th Revised Edition, Version 2, 1994 | |
| 30 | GCVS, 4th edition |
| Kholopov, P.N., et al., General Catalogue of Variable Stars, fourth edition, Moscow: Nauka Publishing House, 1985-88 | |
| 31 | CRM' (non-GCVS variable data) |
| Warren, W.H. Jr., Northern Hemisphere Catalog of Red Magnitudes, 1994 | |
| 96 | SAO or HD/HDE Catalog |
| Reference from Value 1 or Reference from Value 2 | |
data from Smithsonian Astrophysical Observatory Star Catalog (SAO Staff 1966; USNO, ADC 1990)
position and proper motion:
| position (J1950) | RA: 5h 21min 57,676sec | DEC: -2° 26' 29,58'' | ±0,014 arcsec |
| position (J2000) | RA: 5h 24min 28,638sec | DEC: -2° 23' 49,38'' | |
| proper motion J1950 (FK4) | RA: -0,0002 arcsec/a | DEC: 0,001 arcsec/a | ±0,002 arcsec/a in RA ±0,002 arcsec/a in DEC |
| proper motion J2000 (FK5) | RA: 0,0001 arcsec/a | DEC: 0 arcsec/a | |
| source of proper motion data | Determined by source catalog | ||
magnitude:
| visual | 3,4 (accuracy: 2 decimals) |
| source of visual magnitude data | Combined magnitude of component stars. |
spectral information:
| spectral class | B1 |
| source of spectral data | Taken from the HD with M stars reclassified by Miss Cannon. |
remarks for duplicity and variability
| Double star - see source catalog for source |
catalogues
| source catalogue | FK3, catalogue number: 200 |
| Durchmusterung | BD-02 1235 |
| Boss General Catalogue | 6655 |
| Henry Draper Catalogue | 35411 |
data from The Washington Visual Double Star Catalog, 1996.0 (Worley+, 1996)
position and proper motion:
| position (J2000) | RA: 5h 24,5min | DEC: -2° 24' |
| proper motion (J2000) | RA: 0,003 arcsec/a | DEC: -0,001 arcsec/a |
double/multiple star system information:
| component | year | number of measures | position angle | angular separation | magnitude of 1st component | magnitude of 2nd component | spectral class(es) | discoverer code |
| Aa | 1975 | 16 | 134° | 0,1'' | 3,36 | - | B1V+B2e | MCA 18 |
| 1988 | 116° | - | ||||||
| Aa-B | 1848 | often | 87° | 1'' | 3,8 | 4,8 | B1V+B2e | DA 5 |
| 1989 | 78° | 1,7'' | ||||||
| Aa-C | 1904 | 3 | 51° | 115,1'' | 3,4 | 9,4 | B1V+B2e | H 67 |
| 1977 | 52° | 116,1'' |
discoverer information:
| discoverer code | discoverer | reference |
| MCA 18 | McAlister, H.A. | (Astron. J. 106, 1639; 1993.) |
| DA 5 | Dawes, W.R. | - |
| H 67 | Herschel, W. | - |
notes:
| note | Eta Ori. A is a spectroscopic and eclipsing binary, P = 7.99d. A has been resolved into a third component by speckle interferometry. A spectroscopic period of 9.51y has been determined. H VI 67. |
data from Combined General Catalogue of Variable Stars (Vol. I-III) (Kholopov+ 1998)
position:
| position (J1950) | RA: 5h 21min 57,7sec | DEC: -2° 26' 30'' |
variability informations:
| variability type | EA+BCEP: | close binary eclipsing system pulsating variable star |
| magnitute at max. brightness | 3,31 | |
| magnitute at min. brightness | 3,6 | |
| photometric system | visual, photovisual or Johnson's V | |
| epoch for maximum light [JD] | 2415761,826 12. January 1902, 07:49:26 UT |
|
| period [d] | 7,989268 | |
| next maximum light [JD] | 2451625,650052 22. March 2000, 03:36:04 UT |
spectral information
| spectral class | B0.5Vea+B3V |
references
| to a study | Vol. II GCVS |
| to a chart/photograph | Vol. I GCVS (see Kholopov et al. 1985-1988) |
miscanellous
| ID in the GCVS catalogue | 60/9007 |
| constellation | Orion |
| notes on existence | The star is equivalent to '06090151omi 1'. |
| There are notes in published catalog. | |
variability type description
| variability type | description |
| EA | Eclipsing binary systems. These are binary systems with orbital planes so close to the observer's line of sight (the inclination i of the orbital plane to the plane orthogonal to the line of sight is close to 90 deg) that the components periodically eclipse each other. Consequently, the observer finds changes of the apparent combined brightness of the system with the period coincident with that of the components' orbital motion. EA Algol (Beta Persei)-type eclipsing systems. Binaries with spherical or slightly ellipsoidal components. It is possible to specify, for their light curves, the moments of the beginning and end of the eclipses. Between eclipses the light remains almost constant or varies insignificantly because of reflection effects, slight ellipsoidality of components, or physical variations. Secondary minima may be absent. An extremely wide range of periods is observed, from 0.2 to >= 10000 days. Light amplitudes are also quite different and may reach several magnitudes. EB Beta Lyrae-type eclipsing systems. These are eclipsing systems having ellipsoidal components and light curves for which it is impossible to specify the exact times of onset and end of eclipses because of a continuous change of a system's apparent combined brightness between eclipses; secondary minimum is observed in all cases, its depth usually being considerably smaller than that of the primary minimum; periods are mainly longer than 1 day. The components generally belong to early spectral types (B-A). Light amplitudes are usually <2 mag in V. EW W Ursae Majoris-type eclipsing variables. These are eclipsers with periods shorter than 1 days, consisting of ellipsoidal components almost in contact and having light curves for which it is impossible to specify the exact times of onset and end of eclipses. The depths of the primary and secondary minima are almost equal or differ insignificantly. Light amplitudes are usually <0.8 mag in V. The components generally belong to spectral types F-G and later. |
| BCEP | Variables of the Beta Cephei type (Beta Cep, Beta CMa), which are pulsating O8-B6 I-V stars with periods of light and radial-velocity variations in the range of 0.1 - 0.6 days and light amplitudes from 0.01 to 0.3 mag in V. The light curves are similar in shape to average radial-velocity curves but lag in phase by a quarter of the period, so that maximum brightness corresponds to maximum contraction, i.e., to minimum stellar radius. The majority of these stars probably show radial pulsations, but some (V649 Per) display nonradial pulsations; multiperiodicity is characteristic of many of these stars. |