New variable star in Vela
نویسندگان
چکیده
منابع مشابه
Luminous Red Variable Star
We report photometry and spectroscopy of the evolution of Nova Sagittarii 1994 #1 (V4332 Sagittarii) during outburst. We compare the photometric and spectral evolution of this outburst to known classes of outbursts – including classical novae and outbursts occurring on symbiotic stars – and find this object does not conform to any known class of outburst. The closest match to the behavior of th...
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We study the association between embedded star clusters and young stellar objects believed to be precursors of intermediate mass stars (2 <∼ M <∼ 10 M ), within the Vela Molecular Ridge D-cloud. A sample of 12 IRAS-selected Class I sources belonging to the region was imaged in the near infrared bands JHK and the photometry used in order to gain information on the stellar population around these...
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We present the results of a Near-Infrared deep photometric survey of a sample of six embedded star clusters in the Vela-D molecular cloud, all associated with luminous (∼ 10 3 L ⊙) IRAS sources. The clusters are unlikely to be older than a few 10 6 yrs, since all are still associated with molecular gas. We employed the fact that all clusters lie at the same distance and were observed with the s...
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There are currently two well-accepted models that explain how pulsars exhibit glitches, sudden changes in their regular rotational spin-down. According to the starquake model, the glitch healing parameter, Q, which is measurable in some cases from pulsar timing, should be equal to the ratio of the moment of inertia of the superfluid core of a neutron star (NS) to its total moment of inertia. Me...
متن کاملNeutron star sequences and the starquake glitch model for the Crab and the Vela pulsars
We construct for the first time, the sequences of stable neutron star (NS) models capable of explaining simultaneously, the glitch healing parameters, Q, of both the pulsars, the Crab (Q ≥ 0.7) and the Vela (Q ≤ 0.2), on the basis of starquake mechanism of glitch generation. These models yield an upper bound on surface redshift of NSs, zR ≃ 0.77. If the lower limit of the observational constrai...
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ژورنال
عنوان ژورنال: Astronomische Nachrichten
سال: 1894
ISSN: 0004-6337,1521-3994
DOI: 10.1002/asna.18941350305