q1Orionis


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

  2. SKY2000 - Master Star Catalog

  3. The Washington Visual Double Star Catalog, 1996.0

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


catalogues and names q1Ori, V1016 Ori, 41 Ori, HR 1893, HD 37020, WDS 05354-0525A
constellation Orion

data from The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version) (Hoffleit+, 1991)


position, motion, parallax:

position (J2000) RA: 5h 35min 15,9sec DEC: -5 23' 14''
position (J1900) RA: 5h 30min 21sec DEC: -5 27' 12''
proper motion (J2000) RA: 0,005 arcsec/a DEC: 0,002 arcsec/a
radial velocity 32 km/s
note: spectroscopic binaries
note: orbital data avaible
rotational velocity 112 km/s (uncertain) (variable)
trigonometric parallax 0,001 arcsec

magnitude

visual magnitude 6,73
(V on UBV Johnson system)

spectral / color information

spectral class B0.5V
B-V-magnitude 0,02
U-B-magnitude -0,88
R-I-magnitude 0,21
note (category: spectra): Also classified B0.5Vp.
note (category: colors): Abnormal reddening at 1500A. IR source.

variability information

variable star identification V1016 Ori
note (category: variability): ADS 4186A, EA, 6.72 - 6.75V, 65.43233d. Component E is NSV 2291, amp. 0.41V; component F is NSV 2296, 11.0V; component H is NSV 2292, 15.6V.

double/multiple star system information

number of components of multiple star system 12
separation 117 arcsec
mag difference (of double or brightest multiple) 0,1
component ID *
note (category: double and multiple data): ADS 4186AC fixed at 13". C = HR 1895. ADS 4186 and 4188 together appear to form one complex multiple system whose brightest components are ADS 4186C = HR 1895 and ADS 4188A = HR 1897. These two components are double star STF 17 which IDS lists as part of ADS 4188. Thus, the 9 components of ADS 4186 and the 4 of ADS 4188 form one system of at least 12 components. Those of ADS 4186 range from mag. 5.4 to 16.7v, all within 22" of A. ADS 4188 has two other companions in addition to HR 1895: B, 6.5v at 53" and C, 7.6v at 129" from HR 1897.
note (category: spectroscopic binaries): 65.43233d, K 33.3k/s, V0 +13.3k/s.

miscellaneous information

note (category: group membership): Ori OB1d; sword of Orion; a trapezium star.

data from SKY2000 - Master Star Catalog (Myers+ 1997)

position, motion, parallax:

position (J2000) RA: 5h 35min 15,829sec DEC: -5 23' 14,28'' 0,5 arcsec source: 25
proper motion (J2000) RA: 0,0003 arcsec/a DEC: 0,002 arcsec/a source: 25
radial velocity 32 km/s source: 25
trigonometric parallax 0,001 - source: 25
galactic coord. (B1950) longitude: 209,01 latitude: -19,39
GCI unit vector (J2000) X: 0,107247 Y: 0,98979 Z: -0,093888

magnitude:

visual 6,73 (observed) source: 20
photovisual 6,8 source: 2

spectral information:

spectral class B5 source: 24
Morgan-Keenan B0.5V source: 25
B-magnitude 6,75 0,018 B-V-magnitude 0,02
U-magnitude 5,85 0,043 U-B-magnitude -0,9

variability information:

source of data: 30
variability type 310
var. amplitude 0,93
var. period 65,43
var. epoch 2443145
1. January 1977, 12:00:00 UT
next max light 2451650,9
16. April 2000, 09:36:00 UT

double/multiple star system information:

source of data: 19
separation between brightest and second brightest component 8,8 arcsec
position angle 32

component magnitude spectral class catalogue(s)/name(s)
A 6,73 B5 q1Orionis, 41 Ori, HR 1893, HD 37020,
B 5,13 O0 q1Orionis, 41 Ori, HR 1895, HD 37022, SAO 132314
C 6,7 BO q1Orionis, 41 Ori, HR 1896, HD 37023,

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
19 WDS Catalog
Worley, C.E., and G.G. Douglass, Washington Catalog of Visual Double Stars 1996.0, United States Naval Observatory, 1996
20 Catalogue of Homogeneous Means in the UBV System
Mermilliod, J.C., Catalogue of Homogeneous Means in the UBV System, Institut d'Astronomie, Universite de Lausanne, 1994
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

data from The Washington Visual Double Star Catalog, 1996.0 (Worley+, 1996)

position and proper motion:

position (J2000) RA: 5h 35,4min DEC: -5 25'
proper motion (J2000) RA: 0,003 arcsec/a DEC: 0,002 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
AB 1836 19 92 52,5'' 5,07 6,39 O9.5Vep STF 16
AC 1869 5 98 128,7'' 5,2 9,1 - STF 16
- 1836 9 314 135'' 4,9 5 - STF 17

discoverer information:

discoverer code discoverer reference
STF 16 Struve, F.G.W. -
STF 17 Struve, F.G.W. -

notes:

note Theta (2) Ori. B is BD-05@ 1320. Proper motion of B +013 +015. A is a spectroscopic binary, P = 21d.

data from Combined General Catalogue of Variable Stars (Vol. I-III) (Kholopov+ 1998)

position:

position (J1950) RA: 5h 32min 48sec DEC: -5 25' 6'' 1 sec / 0.1 arcmin

variability informations:

variability type EA close binary eclipsing system
magnitute at max. brightness 6,72
magnitute at min. brightness 7,65
photometric system visual, photovisual or Johnson's V
epoch for maximum light [JD] 2443144,6
1. January 1977, 02:24:00 UT
period [d] 65,43233
next maximum light [JD] 2451650,8029
16. April 2000, 07:16:11 UT
duration of the eclipse 01 % of period

spectral information

spectral class B0.5Vp

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 60/1016
constellation Orion
notes on existence The star is equivalent to '0601017 V1017'.
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.