Contents
Images
Upload your image
DSS Images Other Images
Related articles
NP Pavonis : Differential Corrections Analysis of the UBV Observations
The first photoelectric analysis of the NPbinary system based on U, B,and V light curves and modeled using the Wilson & Devinney approach,is presented. The light curves are defined by 3861 individualobservations. The components and the orbit appears to be in generalstable. The primary, more massive, more luminous is the greatercomponent, eclipsed at primary minimum and is detached from its Rochelobe (94%). The secondary nearly fills its Roche lobe (99%) and has atemperature difference of Delta = - 1330^oK. The absolute elements wereobtained supposing that the primary follows the mass-luminosityrelation.
| The Active Algol Binary KZ Pavonis
The Algol type eclipsing binary KZ Pav has been observed over onecomplete orbit (0.95 days) with theAustralia Telescope CompactArray.Contemporaneous optical photometric data from the University of SouthernQueensland's Observatory at Mount Kent were also collected and have beenincluded in this multi-wavelength study. Preliminary indications arethat the low levels of emission observed share similarities to those ofsome RS CVn binaries. The optical data show phase-linked effects whichcan be related to the mass transfer process of Algols. The possibilitythat the radio emission may be related to this process is considered.
| First Determinations of Photoelectric Minima, Real Period and Study of the Period of NP Pav
The real period of this binary was determined when the light curve wascompleted. Between the photographic and photoelectric minima the periodremains in first approximation constant.
| The eclipsing binary system KZ Pav
Not Available
| Behavior of the CA II-K line in the cool AP star HD 197417
The southern cool peculiar star HD 197417 shows a large variation in thephotometric index c1. Spectroscopic investigations point outvariations in the profile and equivalent width of the Ca II-K line,which are correlated with those of the Sr II, Eu II, Fe II and Cr IIlines. The possibility that this periodic behavior of the Ca II-K linemay be due to UV blanketing or to diffusion effects is investigated. Theappearance of wings at the maximum of intensity of the Ca II-K line isdiscussed.
|
Submit a new article
Related links
Submit a new link
Member of following groups:
|
Observation and Astrometry data
| Constellation: | Ταώς |
| Right ascension: | 20h58m11.68s |
| Declination: | -69°08'46.4" |
| Apparent magnitude: | 6.831 |
| Distance: | 165.837 parsecs |
| Proper motion RA: | 15.8 |
| Proper motion Dec: | -29.5 |
| B-T magnitude: | 6.767 |
| V-T magnitude: | 6.826 |
Catalogs and designations:
|
