Propus


The object was found in the following catalogues:
  1. The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version)

  2. SKY2000 - Master Star Catalog

  3. Smithsonian Astrophysical Observatory Star Catalog

  4. The Washington Visual Double Star Catalog, 1996.0

  5. Combined General Catalogue of Variable Stars (Vol. I-III)


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.

object is infrared source (NASA merged infrared catalogue, Schmitz et al., 1978)

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:

source of data: 30
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:

source of data: 19
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.