Shaula
| catalogues and names | Shaula, l Sco, lam Sco, 35 Sco, HR 6527, HD 158926, SAO 208954, FK5: 652, WDS 17336-3706A |
| constellation | Scorpius |
data from The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version) (Hoffleit+, 1991)
| note (category: star names): | SHAULA. |
position, motion, parallax:
| position (J2000) | RA: 17h 33min 36,5sec | DEC: -37° 6' 14'' |
| position (J1900) | RA: 17h 26min 49sec | DEC: -37° 1' 51'' |
| proper motion (J2000) | RA: -0,001 arcsec/a | DEC: -0,029 arcsec/a |
| radial velocity | -3 km/s note: spectroscopic binaries, double lined spectra |
|
| rotational velocity | 163 km/s (uncertain) (variable) | |
magnitude
| visual magnitude | 1,63 (V on UBV Johnson system) |
spectral / color information
| spectral class | B2IV+B |
| B-V-magnitude | -0,22 |
| U-B-magnitude | -0,89 |
| R-I-magnitude | -0,28 |
| note (category: spectra): | Lyman alpha and Lyman beta observed from COPERNICUS. |
| note (category: colors): | Color excess E(B-V) = +0.03. |
variability information
| variable star identification | Lam Sco |
| note (category: variability): | Beta C 1.59 - 1.65V, 0.2137015d, secondary 0.1068518d, beat period 10.1605d. Also possible 0.04V eclipse. X-ray flare observed in vicinity Lambda Sco on 1 June 1975. |
double/multiple star system information
| number of components of multiple star system | 3 |
| separation | 94,9 arcsec |
| mag difference (of double or brightest multiple) | 10,3 |
| component ID | AC |
| note | Worley (1978) update of the IDS |
| note (category: spectroscopic binaries): | 5.6d. Interferometer measures indicate multiple star. |
miscellaneous information
| note (category: group membership): | Sco-Cen assoc. |
data from SKY2000 - Master Star Catalog (Myers+ 1997)
position, motion, parallax:
| position (J2000) | RA: 17h 33min 36,534sec | DEC: -37° 6' 13,72'' | ±0,06 arcsec | source: 15 |
| proper motion (J2000) | RA: -0,0001 arcsec/a | DEC: -0,029 arcsec/a | source: 25 | |
| radial velocity | -3 km/s | source: 25 | ||
| galactic coord. (B1950) | longitude: 351,75° | latitude: -2,21° | ||
| GCI unit vector (J2000) | X: -0,091637 | Y: -0,792262 | Z: -0,603261 | |
magnitude:
| visual | 1,62 (observed) | source: 30 |
| photovisual | 1,7 | source: 2 |
| photographic | 1,5 | source: 2 |
spectral information:
| spectral class | B2 | source: 96 | |
| Morgan-Keenan | B2IV+B | source: 25 | |
| B-magnitude | 1,41 ±0,05 | B-V-magnitude | -0,22 |
| U-magnitude | 0,52 ±0,05 | U-B-magnitude | -0,89 |
variability information:
| variability type | 10 |
| var. amplitude | 0,06 |
| var. period | 0,21 |
| var. epoch | 2440000 23. May 1968, 12:00:00 UT |
| next max light | 2451622,03 18. March 2000, 12:43:12 UT |
double/multiple star system information:
| separation between brightest and second brightest component | 41,7 arcsec |
| magnitude difference between brightest and second brightest component | 13,3 |
| position angle | 109 ° |
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 | |
| 15 | FK5, FK5 Extension and FK5 Supplement |
| Fricke, W., H. Schwan and T. Lederle, "Fifth Fundamental Catalogue (FK5), Part I. The Basic Fundamental Stars," Veroff. Astronomisches Recheninstitut, No. 32, Heidelberg, Germany, 1988, and Fricke, W., H. Schwan, and T.E. Corbin, "Fifth Fundamental Catalogue (FK5), Part II. The FK5 Extension," Veröff. Astronomisches Recheninstitut, No. 33, Heidelberg, Germany, 1991 | |
| 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 | |
| 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: 17h 30min 12,626sec | DEC: -37° 4' 9,63'' | ±0,009 arcsec |
| position (J2000) | RA: 17h 33min 36,551sec | DEC: -37° 6' 13,61'' | |
| proper motion J1950 (FK4) | RA: 0,0001 arcsec/a | DEC: -0,029 arcsec/a | ±0,002 arcsec/a in RA ±0,002 arcsec/a in DEC |
| proper motion J2000 (FK5) | RA: 0,0001 arcsec/a | DEC: -0,028 arcsec/a | |
| source of proper motion data | Determined by source catalog | ||
magnitude:
| visual | 1,7 (accuracy: 2 decimals) |
| source of visual magnitude data | Taken from the "Henry Draper Catalogue". |
spectral information:
| spectral class | B2 |
| source of spectral data | Taken from the Henry Draper Catalogue or no spectrum in source catalog. |
catalogues
| source catalogue | FK4, catalogue number: 652 |
| Durchmusterung | CD-3711673 |
| Boss General Catalogue | 23769 |
| Henry Draper Catalogue | 158926 |
data from The Washington Visual Double Star Catalog, 1996.0 (Worley+, 1996)
position and proper motion:
| position (J2000) | RA: 17h 33,6min | DEC: -37° 6' |
| proper motion (J2000) | RA: -0,001 arcsec/a | DEC: -0,029 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 | 1897 | 1 | 109° | 41,7'' | 1,6 | 14,9 | B2IV+B | SEE 334 |
| AC | 1897 | 1 | 331° | 94,9'' | 1,6 | 12 | - | DUN 218 |
discoverer information:
| discoverer code | discoverer | reference |
| SEE 334 | See, T.J. | - |
| DUN 218 | Dunlop, J. | - |
notes:
| note | Lambda Sco. Variable. Spectroscopic binary. |
data from Combined General Catalogue of Variable Stars (Vol. I-III) (Kholopov+ 1998)
position:
| position (J1950) | RA: 17h 30min 12,6sec | DEC: -37° 4' 10'' |
variability informations:
| variability type | BCEP+E: | pulsating variable star close binary eclipsing system |
| magnitute at max. brightness | 1,62 | |
| magnitute amplitude | 0,06 | |
| photometric system | visual, photovisual or Johnson's V | |
| epoch for maximum light [JD] | 2440000,1235 23. May 1968, 14:57:50 UT |
|
| period [d] | 0,2136966 | |
| next maximum light [JD] | 2451622,013091 18. March 2000, 12:18:51 UT |
spectral information
| spectral class | B1.5IV |
references
| to a study | Vol. III GCVS |
| to a chart/photograph | no chart is avaible, but the star is contained in the 'Cordoba Durchmusterung' |
miscanellous
| ID in the GCVS catalogue | 73/9011 |
| constellation | Scutum |
| notes on existence | The star is equivalent to '07390121mu 1'. |
| There are notes in published catalog. | |
variability type description
| variability type | description |
| 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. |
| E | 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. |