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HD 33467


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Some remarks on the origin of the abundance anomalies in HgMn stars.
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An Einstein Observatory SAO-based catalog of B-type stars
About 4000 X-ray images obtained with the Einstein Observatory are usedto measure the 0.16-4.0 keV emission from 1545 B-type SAO stars fallingin the about 10 percent of the sky surveyed with the IPC. Seventy-fourdetected X-ray sources with B-type stars are identified, and it isestimated that no more than 15 can be misidentified. Upper limits to theX-ray emission of the remaining stars are presented. In addition tosummarizing the X-ray measurements and giving other relevant opticaldata, the present extensive catalog discusses the reduction process andanalyzes selection effects associated with both SAO catalog completenessand IPC target selection procedures. It is concluded that X-rayemission, at the level of Lx not less than 10 exp 30 ergs/s, is quitecommon in B stars of early spectral types (B0-B3), regardless ofluminosity class, but that emission, at the same level, becomes lesscommon, or nonexistent, in later B-type stars.

Large and kinematically unbiased samples of G- and K-type stars. V - Evolved stars in the selected areas at + 15-deg declination
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1990PASP..102..242E&db_key=AST

Spectral and Luminosity Classification of the Bright Sequence Stars in the C Regions.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1955ApJ...121...32N&db_key=AST

The Transfer of the North Polar Standards to the Southern Hemisphere.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1953ApJ...117...83C&db_key=AST

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Osservazione e dati astrometrici

Costellazione:Orione
Ascensione retta:05h10m59.00s
Declinazione:+14°55'18.5"
Magnitudine apparente:7.929
Distanza:383.142 parsec
Moto proprio RA:-10.7
Moto proprio Dec:-7.2
B-T magnitude:8.057
V-T magnitude:7.94

Cataloghi e designazioni:
Nomi esatti
HD 1989HD 33467
TYCHO-2 2000TYC 710-1136-1
USNO-A2.0USNO-A2 0975-01406282
HIPHIP 24132

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