Results 181 to 190 of about 82,748 (221)
Commodity risk assessment of <i>Vitis</i> spp. plants from Moldova. [PDF]
EFSA JEFSA Panel on Plant Health (PLH) +37 more
europepmc +1 more source
Syntaxonomical Remarks on the Garrigues from Apulia (S Italy) and Neighboring Territories. [PDF]
Plants (Basel)Tomaselli V +8 more
europepmc +1 more source
Dwarf novae in the Hamburg quasar survey: rarer than expected [PDF]
Astronomy and Astrophysics, 2006 Aims. We report the discovery of five new dwarf novae that were spectroscopically identified in the Hamburg Quasar Survey (HQS),and discuss the properties of the sample of new dwarf novae from the HQS. Methods.
Pablo Rodriguez-Gil +2 more
exaly +2 more sources
Data mining for dwarf novae in SDSS, GALEX and astrometric catalogues [PDF]
Monthly Notices of the Royal Astronomical Society, 2010 By cross-matching blue objects from the Sloan Digital Sky Survey with Galaxy Evolution Explorer and the astrometric catalogues USNO-B1.0, GSC2.3 and CMC14, 64 new dwarf nova candidates with one or more observed outbursts have been identified. 14 of these
Boris Gaensicke +2 more
exaly +2 more sources
Transient behaviour of three SU UMa-type dwarf novae: AR Pic, QW Ser, and V521 Peg
Monthly Notices of the Royal Astronomical Society, 2022 Changes in the supercycle lengths of some SU UMa-type dwarf novae have been detected by other studies, and indicate that the mass transfer rates noticeably decrease over time.
Hélène Szegedi, Philip A Charles
exaly +2 more sources
Deriving an X-ray luminosity function of dwarf novae based on parallax measurements [PDF]
Monthly Notices of the Royal Astronomical Society, 2010 We have derived an X-ray luminosity function using parallax-based distance measurements of a set of 12 dwarf novae, consisting of Suzaku, XMM-Newton and ASCA observations.
J R Thorstensen
exaly +4 more sources
A MeerKAT survey of nearby dwarf novae: I. New detections [PDF]
Monthly Notices of the Royal Astronomical SocietyA programme to search for radio emission from dwarf-novae-type cataclysmic variables was conducted with the South African MeerKAT radio telescope. The dwarf novae RU Pegasi, V426 Ophiuchi, and IP Pegasi were detected during outburst at L band (1284 MHz ...
Ian Heywood +2 more
exaly +2 more sources
Some of the next articles are maybe not open access.
Related searches:
Related searches:
The decay of dwarf nova outbursts
Space Science Reviews, 1985Simultaneous observations at different wavelengths of the decay of dwarf-nova outbursts, show an earlier return to the quiescence level at shorter wavelengths. These observations, which show completely new aspects of outbursts, can provide strong tests for outburst models and accretion-disc theory.
H. van der Woerd, J. Heise
openaire +1 more source
Astrophysics, 1999
In searchs for flare stars in the vicinity of the Pleiades cluster, three flares were detected in 1970,1972, and 1977 in a star with the coordinates α1950= 3h48m·9, δl950= 25‡15’.8. The star’s brightness at a minimum is >21m·5. The star was tentatively assigned to the U Gem type.
E. A. Parsamian +2 more
openaire +1 more source
In searchs for flare stars in the vicinity of the Pleiades cluster, three flares were detected in 1970,1972, and 1977 in a star with the coordinates α1950= 3h48m·9, δl950= 25‡15’.8. The star’s brightness at a minimum is >21m·5. The star was tentatively assigned to the U Gem type.
E. A. Parsamian +2 more
openaire +1 more source
Advances in Space Research, 1988
Previous papers have shown that the dwarf nova OY Car has an extensive vertical disk structure during its superoutbursts. This structure is analogous to that seen in the low mass X-ray binaries (LMXBs), in that the whole disk flares toward its edge, and there is a bulge or 'dark spot' where the mass transfer stream meets the disk edge.
T. Naylor +3 more
openaire +1 more source
Previous papers have shown that the dwarf nova OY Car has an extensive vertical disk structure during its superoutbursts. This structure is analogous to that seen in the low mass X-ray binaries (LMXBs), in that the whole disk flares toward its edge, and there is a bulge or 'dark spot' where the mass transfer stream meets the disk edge.
T. Naylor +3 more
openaire +1 more source