Results 11 to 20 of about 49,810 (294)

WZ SGE STARS

Odessa Astronomical Publications, 2007
The WZ Sge type stars is a rare subclass of the cataclysmic variables (CVs). It possesses the properties of both dwarf novae and recurrent novae. The WZ Sge stars have the shortest orbital periods (typically 80 - 90 minutes) known among the dwarf novae ...
E. P. Pavlenko
doaj   +1 more source

The Behavior of Novae Light Curves Before Eruption [PDF]

, 2009
In 1975, E. R. Robinson conducted the hallmark study of the behavior of classical nova light curves before eruption, and this work has now become part of the standard knowledge of novae.
Alcock, Alcock, Alksne, Anderson, Andrew C. Collazzi, Anonymous, Apriamashvili, Arne A. Henden, Ashley Pagnotta, Becker, Beer, Bertaud, Bertiau, Beyer, Bradley E. Schaefer, Bruch, Bruch, Campbell, Campbell, Dinnerstein, Downes, Efremov, Fehrenbach, Fekel, Gessner, Götz, Hassel, Herbig, Hinderer, Hoffleit, Hoffmeister, Honeycutt, Hopp, Kafka, Kałużny, King, Klaus Löchel, Knigge, Kukarkin, Kukarkin, Kürster, Leavitt, Leibowitz, Liller, Liller, Limin Xiao, Lowne, Löchel, Meinunger, Mennickent, Monet, Newsom, Nielsen, Osada, Parenago, Parenago, Peltier, Peltier, Peter Kroll, Pickering, Pickering, Pogson, Prentice, Retter, Rosino, Samus, Sanduleak, Schaefer, Schaefer, Schaefer, Schaefer, Schaefer, Schaefer, Schaefer, Schweitzer, Semeniuk, Shafter, Shafter, Shapley, Shen, Sherrington, Shugarov, Solomon, Starrfield, Tamm, Thomas, Uthas, van Genderen, van Schewick, van Teeseling, Wachmann, Wade, Warner, Warner, Warner, Warner, Wenzel, Whipple, Whipple, Whipple, Xiao, Yonehara   +101 more
core   +3 more sources

The Early Palomar Program (1950-1955) for the Discovery of Classical Novae in M81: Analysis of the Spatial Distribution, Magnitude Distribution, and Distance Suggestion [PDF]

, 1999
Data obtained in the 1950-1955 Palomar campaign for the discovery of classical novae in M81 are set out in detail. Positions and apparent B magnitudes are listed for the 23 novae that were found.
Allan Sandage, Buscombe W., David R. Zurek, Della Valle M., Della Valle M., Hatano K., Holmberg E., Kraft R. P., Kraft R. P., McLaughlin D. B., Metcalfe N., Michael M. Shara, Moses R. N., Prialnik D., Prialnik D., Reimers D., Schmidt Th., Starrfield S., Tully R. B., Weidemann V., Weidemann V.   +20 more
core   +3 more sources

On Super-Novae [PDF]

Proceedings of the National Academy of Sciences, 1934
The extensive investigations of extragalactic systems during recent years have brought to light the remarkable fact that there exist two well-defined types of new stars or novae which might be distinguished as common novae and super-novae. No intermediate objects have so far been observed.
W, Baade, F, Zwicky
openaire   +2 more sources

Nucleation in Novae [PDF]

International Astronomical Union Colloquium, 1987
AbstractWe consider the possibility that dust grains in novae could nucleate on ions. We examine how different ejected masses and different elemental abundances effect the availability of nucleation centres, and we show how this model could explain why only novae of intermediate speed classes form dust.
C. M. Callus, J. S. Albinson, A. Evans
openaire   +2 more sources

Thermonuclear Runaways on Accreting White Dwarfs: Models of Classical Novae Explosions [PDF]

, 2000
The mechanism of classical novae explosions is explained, together with some of their observational properties. The scarce but not null impact of novae in the chemical evolution of the Milky Way is analyzed, as well as their relevance for the ...
Hernanz, Margarita, Jose, Jordi
core   +3 more sources

Nucleosynthesis in Novae [PDF]

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016), 2017
Peer ...
openaire   +2 more sources

Swift X-Ray Observations of Classical Novae. II. The Super Soft Source sample

, 2011
The Swift GRB satellite is an excellent facility for studying novae. Its rapid response time and sensitive X-ray detector provides an unparalleled opportunity to investigate the previously poorly sampled evolution of novae in the X-ray regime. This paper
A. P. Beardmore, Anupama, Anupama, Ayani, Ayani, Ayani, Baklanov, Balman, Balman, Balman, Beardmore, Bode, Bode, Bode, Bode, Bode, Bode, Bos, Boyd, Bruch, Buil, Camilleri, Charles E. Woodward, Chochol, Chochol, Cragg, Czart, della Valle, Diaz, Drake, Drake, Drake, Duerbeck, Duerbeck, Evans, Evans, Ferri, Frederick M. Walter, Fujii, Gilmore, Greg J. Schwarz, Hachisu, Hachisu, Hachisu, Hanzl, Helton, Helton, Helton, Helton, Hernanz, Hernanz, Hernanz, Hirosawa, Hounsell, Iijima, Iijima, J. P. Osborne, Jan-Uwe Ness, Jeremy J. Drake, K. L. Page, Kang, Kato, Kato, Kato, Kato, Kiss, Kiss, Krauss Hartman, Krautter, Krautter, L. Andrew Helton, Lane, Lee, Liller, Liller, Liller, Liller, Liller, Liller, Liller, Liller, Liller, Liller, Liller, Liller, Liller, Lyke, Lynch, Lynch, Lynch, Lynch, Lynch, Lynch, Lynch, Mason, Mazuk, Mazuk, Mike Bode, Munari, Munari, Munari, Munari, Munari, Munari, Munari, Munari, Naito, Naito, Naito, Naito, Naito, Nakano, Nakano, Nakano, Nakano, Nakano, Nakano, Nakano, Nakano, Nakano, Nakano, Nakano, Nakano, Nelson, Nelson, Nelson, Ness, Ness, Ness, Ness, Ness, Ness, Ness, Ness, Ness, Ness, Ness, Nishimura, Nishiyama, O'Brien, O'Brien, O'Brien, Orio, Orio, Osborne, Osborne, Osborne, P. A. Evans, Pagnotta, Pereira, Perry, Pigulski, Pojmanski, Pojmanski, Pojmanski, Pojmanski, Pojmanski, Prieto, Puetter, Rafanelli, Ragan, Rauch, Reinsch, Retter, Ribeiro, Rudy, Rudy, Rudy, Rudy, Rudy, Rudy, Rudy, Russell, Russell, Russell, Russell, Russell, Russell, Russell, Sadakane, Saizar, Sala, Samus, Schaefer, Schaefer, Schlegel, Schlegel, Schlegel, Schwarz, Schwarz, Schwarz, Schwarz, Schwarz, Schwarz, Shafter, Shara, Shore, Shore, Shore, Sitko, Siviero, Siviero, Snijders, Soma, Sostero, Starrfield, Starrfield, Starrfield, Stickland, Stringfellow, Strope, Sugano, Sumner Starrfield, Suzuki, Swierczynski, Takamizawa, Terada, Tomov, Tomov, Tsujimoto, van den Bergh, Vanlandingham, Vanlandingham, Vanlandingham, Vaytet, Waagen, Waagen, Wagner, Walder, Walter, Warner, Whitelock, Williams, Yamaoka, Yamaoka, Yaron   +235 more
core   +1 more source

Pre-maximum and maximum of Novae: The spectroscopic observations of Nova ASASSN-17hx [PDF]

, 2018
The coverage of the pre-maximum stage of novae is sparse, with the exception of a few slow novae where the pre-maximum duration is of the order of some weeks.
Poggiani, Rosa
core   +2 more sources

The Wendelstein Calar Alto Pixellensing Project (WeCAPP): the M31 Nova catalogue

, 2011
We present light curves from the novae detected in the long-term, M31 monitoring WeCAPP project. The goal of WeCAPP is to constrain the compact dark matter fraction of the M31 halo with microlensing observations. As a by product we have detected 91 novae
Baernbantner, O., Bender, R., Fliri, J., Goessl, C., Hopp, U., Lee, C. -H., Ries, C., Riffeser, A., Seitz, S.   +8 more
core   +3 more sources