# Search results for: J. Smak

Acta Astronomica > 2023 > Vol. 73, No. 3 > 227--232

_{1}=0.86±0.18 M

_{☉}, M

_{2}=0.103±0.0022 M

_{☉}, A=1.508±0.100×10

^{10}cm, and i=69±3°. The secondary component of the system is a semi-degenerate helium star loosing mass at a rate M=4.93±1.65×10

^{-9}M

_{☉}/yr. The accretion disk is sufficiently hot to avoid thermal instability. The orbital light curve recovered from observations made in 1962 shows minimum shifted to phase...

Acta Astronomica > 2022 > Vol. 72, No. 1 > 21--29

^{-10}in 1962 to -(5.44±0.61)× 10

^{-10}in 2022. This implies that the mass transfer from the secondary component is accelerating. From the evidence based on the orbital period variations, combined with estimates of the mass loss from the system based on radio observations, it follows that (1) the mass transfer...

Acta Astronomica > 2020 > Vol. 70, No. 4 > 317--321

Acta Astronomica > 2020 > Vol. 70, No. 4 > 313--315

_{crit}=0.22, i.e. smaller than obtained earlier by other authors (q

_{crit}=0.25-0.39). This implies that the tidal-resonance model fails to explain superhumps in systems with orbital...

Acta Astronomica > 2019 > Vol. 69, No. 1 > 79--85

_{2}and V

_{2,rot}sin i and q (estimated from P

_{nSH}), are M

_{1}=0.60±0.20 M☉, M

_{2}=0.48±0.15 M☉, A=1.13±0.09×1011 cm and i=72°.5±2°.5.

Acta Astronomica > 2017 > Vol. 67, No. 3 > 273--280

_{SH}, and the amplitudes of the periodic light variations with the beat period - the irradiation amplitudes - A

_{irr}. The resulting values of A

_{SH}and A

_{irr}, together with other values from the literature, turn out to be correlated thereby confirming the irradiation modulated mass transfer...

Acta Astronomica > 2017 > Vol. 67, No. 1 > 63--69

Acta Astronomica > 2016 > Vol. 66, No. 1 > 75--83

Acta Astronomica > 2014 > Vol. 64, No. 2 > 167--175

Chemical Physics Letters > 2013 > 583 > Complete > 74-79

_{2}as high-k gate dielectric on n-GaAs...

Veterinary Immunology and Immunopathology > 2013 > 151 > 1-2 > 147-156

Acta Astronomica > 2013 > Vol. 63, No. 3 > 369--377

Acta Astronomica > 2013 > Vol. 63, No. 4 > 453--463

_{nSH}and the amplitudes A

_{beat}of the modulation with the beat period P

_{beat}. Both amplitudes are shown to vary considerably from one season to another. Three correlations are found: (1) between...

Acta Astronomica > 2013 > Vol. 63, No. 1 > 109--114

Acta Astronomica > 2012 > Vol. 62, No. 2 > 213--217

_{s}(egress)<r

_{s}(ingress). This is interpreted as being due to the effects of stream overflow...

Acta Astronomica > 2011 > Vol. 61, No. 1 > 59--69

Acta Astronomica > 2010 > Vol. 60, No. 1 > 83--89

_{tr}=16.8±0.3. This is safely below the critical mass transfer rates of log M

_{crit}=18.1 (corresponding to log T

_{crit}

^{0}=3.88) or log M

_{crit}=17.2 (corresponding to the "revised" value of log T

_{crit}

^{0}=3.65). The mass transfer rate during outbursts is strongly enhanced.

Acta Astronomica > 2010 > Vol. 60, No. 4 > 357--371

_{0}≈0.25 mag, while at higher inclinations they increase from A

_{0}≈0.3 mag to A

_{0}≈0.6 mag. The mean maximum superhump amplitudes normalized to the average luminosity of the disk are: <A

_{n}>=0.34±0.02 mag in low inclination systems and...

Acta Astronomica > 2009 > Vol. 59, No. 4 > 419--430

Acta Astronomica > 2009 > Vol. 59, No. 1 > 103--107