PU Puppis

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

note (category: star names):

m Pup. Originally called Pi in Bayer and Argelander. Called m in Lacaille (1763) and Baily. Another star HR 2773, also called Pi in Argelander, is the currently accepted star of this designation.

position, motion, parallax:

position (J2000)	RA: 7h 38min 18sec	DEC: -25° 21' 53''
position (2000.73)	RA: 7h 38min 20sec	DEC: -25° 21' 59''
position (B1900)	RA: 7h 34min 8.2sec	DEC: -25° 8' 16''
proper motion (J2000)	RA: -0.007 arcsec/a	DEC: -0.007 arcsec/a
radial velocity	41 km/s note: variable radial velocity
rotational velocity	293 km/s
galactic coordinates	longitude: 240.65°	latitude: -1.84°

magnitude

visual magnitude

4.7
(V on UBV Johnson system)

spectral / color information

spectral class	B8IV
B-V-magnitude	-0.11
U-B-magnitude	-0.35
R-I-magnitude

variability information

variable star identification

PU Pup

note (category: variability):

EW amp. 0.06V, 2.57895d.

double/multiple star system information

separation	0.2 arcsec
mag difference (of double or brightest multiple)	0.4

note (category: double and multiple data):

Unresolved by speckle interferometry.

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

position, motion, parallax:

position (J2000)	RA: 7h 38min 18.072sec	DEC: -25° 21' 53.61''	ą0.19 arcsec	source: 16
position (2000.73)	RA: 7h 38min 20sec	DEC: -25° 22' 0''	JD: 2451810.11
proper motion (J2000)	RA: 0.0006 arcsec/a	DEC: -0.017 arcsec/a		source: 25
radial velocity	41 km/s			source: 25
galactic coord. (B1950)	longitude: 240.66°	latitude: -1.84°

magnitude:

visual	4.69 (observed)	source: 30
photovisual	3.8	source: 16
photographic	4.6	source: 2

spectral information:

spectral class	B8		source: 96
Morgan-Keenan	B8IV		source: 25
B-magnitude	4.59 ą0.05	B-V-magnitude	-0.11
U-magnitude	4.24 ą0.05	U-B-magnitude	-0.35

variability information:

source of data: 30

variability type	320
var. amplitude	0.06
var. period	2.58
var. epoch	2443100 17. November 1976, 12:00:00 UT
next max light	2451812.66 25. September 2000, 03:50:24 UT

double/multiple star system information:

source of data: 19

separation between brightest and second brightest component	0.1 arcsec
magnitude difference between brightest and second brightest component	0.2

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
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 (B1950)	RA: 7h 36min 13.084sec	DEC: -25° 15' 0.43''	ą0.027 arcsec
position (2000.73)	RA: 7h 38min 20sec	DEC: -25° 21' 59''	JD: 2451810.11
position (J2000)	RA: 7h 38min 18.001sec	DEC: -25° 21' 53.46''
proper motion B1950 (FK4)	RA: -0.0008 arcsec/a	DEC: -0.01 arcsec/a	ą0.005 arcsec/a in RA ą0.005 arcsec/a in DEC
proper motion J2000 (FK5)	RA: -0.0005 arcsec/a	DEC: -0.007 arcsec/a
source of proper motion data	Determined by source catalog

magnitude:

visual	4.6 (accuracy: 2 decimals)
source of visual magnitude data	Taken from Harvard or San Luis photometry.

spectral information:

spectral class	B8
source of spectral data	Taken from the Henry Draper Catalogue or no spectrum in source catalog.

remarks for duplicity and variability

Double star in Aitken's Double Star Catalogue (Aitken 1932)

catalogues

source catalogue	GC, catalogue number: 10266
Durchmusterung	CD-25 4828
Boss General Catalogue	10266
Henry Draper Catalogue	61429

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

position and proper motion:

position (J2000)	RA: 7h 38.3min	DEC: -25° 22'
proper motion (J2000)	RA: -0.001 arcsec/a	DEC: -0.005 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
-	1926	11	°	0.1''	5.4	5.6	B8IV	B 731

discoverer information:

discoverer code	discoverer	reference
B 731	Bos, W.H. van den	-

notes:

note	Duplicity still not certain. Needs speckle.

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

position:

position (equinox 1950.0)

RA: 7h 36min 13.1sec

DEC: -25° 15' 0''

variability informations:

variability type	EB	close binary eclipsing system
magnitute at max. brightness	4.69
magnitute at min. brightness	4.75
photometric system	visual, photovisual or Johnson's V
epoch for maximum light [JD]	2443100 17. November 1976, 12:00:00 UT
period [d]	2.57895
next maximum light [JD]	2451811.6931 24. September 2000, 04:38:04 UT

spectral information

spectral class

references

to a study	Vol. I GCVS (see Kholopov et al. 1985-1988)
to a chart/photograph	no chart is avaible, but the star is contained in the 'Cordoba Durchmusterung'

miscanellous

ID in the GCVS catalogue	68/319
constellation	Puppis
notes on existence	The star is equivalent to '0680320 PV'.
There are notes in published catalog.

variability type description

variability type

description

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.