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14 Canis Minoris, also known as HD 65345, is a single star in the equatorial constellation of Canis Minor. It is faintly visible to the naked eye with an apparent visual magnitude of +5.30. The distance to this star, as determined from an annual parallax shift of 13.50±0.34 mas, is approximately 242 light years. 14 CMI has a relatively large proper motion, traversing the celestial sphere at the rate of 0.188 arcsecond/year. It is moving further from the Sun with heliocentric radial velocity of +42.6 km/s.
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R Boötis is a variable star in the northern constellation of Boötes. Typically the star is too faint to be readily visible to the naked eye, with a brightness that fluctuates between apparent visual magnitudes of 9.98. The distance to this star is approximately 2,150 light years based on parallax measurements. It is drifting closer with a radial velocity of about −58 km/s.
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Amina Helmi is an Argentine astronomer and professor at the Kapteyn Astronomical Institute at the University of Groningen in the Netherlands.
V1315 Aquilae is a cataclysmic variable star in the north of the equatorial constellation of Aquila. It is in the sub-set of nova-like (NL) variables, specifically a SW Sextantis star. These were characterized as having non-magnetic white dwarfs – thus that do not undergo dwarf-nova bright luminations ("eruptions"). There is countering evidence for some magnetism. Being a SW Sextantis star, V1315 Aquilae has a high rate of mass transfer, so it is in steady-state accretion and in a constant state of outburst. It emits most of its light in the visible range, and this comes from the accretion disk. The eclipse depth is 1.8 mag. No description of the donor star is made.
NGC 1276 is an optical double star system located in the constellation Perseus. The system was discovered by astronomer John Dreyer on December 12, 1876. The pair consists of two 15th magnitude stars known as Pul -3 270349 and Pul -3 270357 that are unrelated as they lie at different distances from each other. Pul -3 270349 lies at a distance of 1,134.5587 parsecs (3,700.436 ly) and Pul -3 270357 lies at a distance of 1,774.6229 parsecs (5,788.046 ly).
References
- ↑ "Curriculum vitae" (PDF). Leiden University.
- ↑ "Nature's 10". www.nature.com. Retrieved 2019-12-20.
- ↑ "Anthony Brown - Leiden University". University of Leiden. Retrieved 19 December 2019.
- ↑ "Anthony Brown". ESA. Retrieved 19 December 2019.
- ↑ Gaia Collaboration; Brown, A. G. A.; Vallenari, A.; Prusti, T.; de Bruijne, J. H.J.; Mignard, F.; Drimmel, R.; Babusiaux, C.; Bailer-Jones, C. A.L.; Bastian, U.; Biermann, M. (November 2016). "Gaia Data Release 1: Summary of the astrometric, photometric, and survey properties". Astronomy & Astrophysics. 595: A2. arXiv: 1609.04172 . Bibcode:2016A&A...595A...2G. doi: 10.1051/0004-6361/201629512 . ISSN 0004-6361.
- ↑ Brown, A. G. A.; Vallenari, A.; Prusti, T.; Bruijne, J. H. J. de; Babusiaux, C.; Bailer-Jones, C. a. L.; Biermann, M.; Evans, D. W.; Eyer, L.; Jansen, F.; Jordi, C. (2018-08-01). "Gaia Data Release 2 - Summary of the contents and survey properties". Astronomy & Astrophysics. 616: A1. arXiv: 1804.09365 . Bibcode:2018A&A...616A...1G. doi: 10.1051/0004-6361/201833051 . ISSN 0004-6361.
- ↑ "Anthony Brown gives prestigious lecture series in Princeton - Leiden University". Leiden University. Retrieved 19 December 2019.
- ↑ "Spitzer Lectures 2019". Department of Astrophysical Sciences, Princeton University. Retrieved 19 December 2019.
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