Propus
| catalogues and names | Propus, h Gem, eta Gem, 7 Gem, HR 2216, HD 42995, SAO 78135, WDS 06149+2230 |
| other names | Praepes, Tejat Prior |
| constellation | Gemini |
data from The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version) (Hoffleit+, 1991)
| note (category: star names): | Propus; Praepes; Tejat Prior. |
position, motion, parallax:
| position (J2000) | RA: 6h 14min 52,6sec | DEC: +22° 30' 24'' |
| position (J1900) | RA: 6h 8min 50,4sec | DEC: +22° 32' 9'' |
| proper motion (J2000) | RA: -0,068 arcsec/a | DEC: -0,012 arcsec/a |
| radial velocity | 19 km/s note: spectroscopic binaries note: orbital data avaible |
|
| trigonometric parallax | 0,014 arcsec | |
| note (category: dynamical parallaxes): | 0.007". |
magnitude
| visual magnitude | 3,28 (V on UBV Johnson system) |
spectral / color information
| spectral class | M3III |
| B-V-magnitude | 1,6 |
| U-B-magnitude | 1,66 |
| R-I-magnitude | 1,31 |
variability information
| variable star identification | Eta Gem |
| note (category: variability): | ADS 4841A, SRa + EA 3.15 - 3.9v, 232.9d. Deepest min. satisfy SB period 2984d. |
double/multiple star system information
| number of components of multiple star system | 3 |
| separation | 0 arcsec |
| mag difference (of double or brightest multiple) | 2 |
| component ID | O |
| note (category: double and multiple data): | AB, 473.7y, a = 1.08". B is 8.8v at 1.4". A is suspected occultation double, 3.4, 5.4v, sep. 0.03". Masses A, 12.4; B, 5.5 solar. The three components are surrounded by a gaseous envelope. |
| note (category: spectroscopic binaries): | ADS 4841A 2983d, K 8.8k/s, V0 +17.6k/s, asini 306. Unresolved by speckle interferometry 1982.17 and 1983.93. |
data from SKY2000 - Master Star Catalog (Myers+ 1997)
position, motion, parallax:
| position (J2000) | RA: 6h 14min 52,703sec | DEC: +22° 30' 24,18'' | ±0,43 arcsec | source: 16 |
| proper motion (J2000) | RA: -0,0042 arcsec/a | DEC: -0,011 arcsec/a | source: 25 | |
| radial velocity | 19 km/s | source: 25 | ||
| trigonometric parallax | 0,014 | ±0,001 arcsec | source: 25 | |
| galactic coord. (B1950) | longitude: 188,86° | latitude: 2,52° | ||
| GCI unit vector (J2000) | X: -0,059932 | Y: 0,921889 | Z: 0,382792 | |
magnitude:
| visual | 3,1 (observed) | source: 31 |
| photographic | 4,5 | source: 16 |
spectral information:
| spectral class | M0 | source: 96 | |
| Morgan-Keenan | M2.5III | source: 25 | |
| B-magnitude | 4,88 ±0,05 | B-V-magnitude | 1,6 |
| U-magnitude | 6,54 ±0,05 | U-B-magnitude | 1,66 |
variability information:
| variability type | 10 |
| var. amplitude | 0,8 |
| var. period | 232,9 |
| var. epoch | 2437725 1. March 1962, 12:00:00 UT |
| next max light | 2451699 3. June 2000, 12:00:00 UT |
double/multiple star system information:
| separation between brightest and second brightest component | 1,5 arcsec |
| position angle | 258 ° |
sources:
| 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: 6h 11min 51,508sec | DEC: +22° 31' 23,36'' | ±0,007 arcsec |
| position (J2000) | RA: 6h 14min 52,649sec | DEC: +22° 30' 24,34'' | |
| proper motion J1950 (FK4) | RA: -0,0048 arcsec/a | DEC: -0,013 arcsec/a | ±0,001 arcsec/a in RA ±0,001 arcsec/a in DEC |
| proper motion J2000 (FK5) | RA: -0,0049 arcsec/a | DEC: -0,012 arcsec/a | |
| source of proper motion data | Determined by source catalog | ||
magnitude:
| visual | 3,7 (accuracy: 1 decimal) |
| source of visual magnitude data | Arithmetic mean of maximum and minimum magnitudes of a variable star |
spectral information:
| spectral class | M0 |
| source of spectral data | Taken from the HD with M stars reclassified by Miss Cannon. |
remarks for duplicity and variability
| Variable star in visual magnitude in source catalog |
catalogues
| source catalogue | FK3, catalogue number: 236 |
| Durchmusterung | BD+22 1241 |
| Boss General Catalogue | 7969 |
| Henry Draper Catalogue | 42995 |
data from The Washington Visual Double Star Catalog, 1996.0 (Worley+, 1996)
position and proper motion:
| position (J2000) | RA: 6h 14,9min | DEC: +22° 30' |
| proper motion (J2000) | RA: -0,069 arcsec/a | DEC: -0,012 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 |
| - | 1881 | 80 | 300° | 1'' | - | 8,8 | M3.5I-II | BU 1008 |
| 1990 | 258° | 1,5'' |
discoverer information:
| discoverer code | discoverer | reference |
| BU 1008 | Burnham, S.W. | - |
notes:
| note | Eta Gem. A is a semi-regular variable. A premature visual orbit has been computed. A is also an occulta- tion binary and a long-period spectroscopic binary. |
data from Combined General Catalogue of Variable Stars (Vol. I-III) (Kholopov+ 1998)
position:
| position (J1950) | RA: 6h 11min 51,5sec | DEC: +22° 31' 23'' |
variability informations:
| variability type | SRA+EA | pulsating variable star close binary eclipsing system |
| magnitute at max. brightness | 3,15 | |
| magnitute at min. brightness | 3,9 | |
| photometric system | visual, photovisual or Johnson's V | |
| epoch for maximum light [JD] | 2437725 1. March 1962, 12:00:00 UT |
|
| period [d] | 232,9 | |
| next maximum light [JD] | 2451699 3. June 2000, 12:00:00 UT |
|
| duration of the eclipse | 50 % of period |
spectral information
| spectral class | M3IIIab |
references
| to a study | Vol. I GCVS (see Kholopov et al. 1985-1988) |
| to a chart/photograph | Vol. I GCVS (see Kholopov et al. 1985-1988) |
miscanellous
| ID in the GCVS catalogue | 38/9007 |
| constellation | Gemini |
| notes on existence | The star is equivalent to '0389012 mu'. |
| There are notes in published catalog. | |
variability type description
| variability type | description |
| SRA | Semiregular variables, which are giants or supergiants of intermediate and late spectral types showing noticeable periodicity in their light changes, accompanied or sometimes interrupted by various irregularities. Periods lie in the range from 20 to >2000 days, while the shapes of the light curves are rather different and variable, and the amplitudes may be from several hundredths to several magnitudes (usually 1-2 mag in V). SRA Semiregular late-type (M, C, S or Me, Ce, Se) giants displaying persistent periodicity and usually small (<2.5 mag in V) light amplitudes (Z Aqr). Amplitudes and light-curve shapes generally vary and periods are in the range of 35-1200 days. Many of these stars differ from Miras only by showing smaller light amplitudes; SRB Semiregular late-type (M, C, S or Me, Ce, Se) giants with poorly defined periodicity (mean cycles in the range of 20 to 2300 days) or with alternating intervals of periodic and slow irregular changes, and even with light constancy intervals (RR CrB, AF Cyg). Every star of this type may usually be assigned a certain mean period (cycle), which is the value given in the Catalogue. In a number of cases, the simultaneous presence of two or more periods of light variation is observed; SRC Semiregular late-type (M, C, S or Me, Ce, Se) supergiants (Mu Cep) with amplitudes of about 1 mag and periods of light variation from 30 days to several thousand days; SRD Semiregular variable giants and supergiants of F, G, or K spectral types, sometimes with emission lines in their spectra. Amplitudes of light variation are in the range from 0.1 to 4 mag, and the range of periods is from 30 to 1100 days (SX Her, SV UMa). |
| 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. |