Add to ORKGWe find an expansion parallax for the slow nova RW UMi (Nova Ursae Minoris 1956). A narrow-band H-alpha image shows that the diameter of the nova shell in 1995 was 2.94(+0.37)(-0.49) arcsec. We derive a distance of 5250(+590)(-1050) pc, and an absolute magnitude at maximum of M-v = -7.7(+0.3)(-0.4) which are consistent with previous estimates for the nova. We also revised known relations between various parameters of nova systems
Aims. We aim to determine individual distances to a small number of rather round, quite regularly sh...
We present the results of a search for nova shells around 101 cataclysmic variables (CVs), using H α...
Hipparcos trigonometrical parallaxes of Mira-type variables have been combined with ground-based ang...
An optical imaging study of recent 30 novae has been undertaken using both ground-based and space-ba...
A search to find spatially resolved nova shells was carried out; two new shells (around FH Ser 1970 ...
Nova shells can provide important information on their distance, their interactions with circumstell...
Eight new spatially resolved nova shells have been found by imaging with a digital detector through ...
Determining reliable distances to classical novae is a challenging but crucial step in deriving thei...
A classical nova is an eruption on the surface of a white dwarf in an accreting binary system. The m...
We have used data obtained with the Fine Guidance Sensors on the Hubble Space Telescope to derive pr...
This thesis focuses on shells ejected during classical nova events. Novae are due to thermonuclear r...
(abridged) Expansion distances (or expansion parallaxes) for classical novae are based on comparing ...
Nova shells are characteristically prolate with equatorial bands and polar caps. Failure to account ...
Over the last decade, nova shells have been discovered around a small number of cataclysmic variable...
A classical nova is an eruption on the surface of a white dwarf in an accreting binary system. The m...
Aims. We aim to determine individual distances to a small number of rather round, quite regularly sh...
We present the results of a search for nova shells around 101 cataclysmic variables (CVs), using H α...
Hipparcos trigonometrical parallaxes of Mira-type variables have been combined with ground-based ang...
An optical imaging study of recent 30 novae has been undertaken using both ground-based and space-ba...
A search to find spatially resolved nova shells was carried out; two new shells (around FH Ser 1970 ...
Nova shells can provide important information on their distance, their interactions with circumstell...
Eight new spatially resolved nova shells have been found by imaging with a digital detector through ...
Determining reliable distances to classical novae is a challenging but crucial step in deriving thei...
A classical nova is an eruption on the surface of a white dwarf in an accreting binary system. The m...
We have used data obtained with the Fine Guidance Sensors on the Hubble Space Telescope to derive pr...
This thesis focuses on shells ejected during classical nova events. Novae are due to thermonuclear r...
(abridged) Expansion distances (or expansion parallaxes) for classical novae are based on comparing ...
Nova shells are characteristically prolate with equatorial bands and polar caps. Failure to account ...
Over the last decade, nova shells have been discovered around a small number of cataclysmic variable...
A classical nova is an eruption on the surface of a white dwarf in an accreting binary system. The m...
Aims. We aim to determine individual distances to a small number of rather round, quite regularly sh...
We present the results of a search for nova shells around 101 cataclysmic variables (CVs), using H α...
Hipparcos trigonometrical parallaxes of Mira-type variables have been combined with ground-based ang...