The continuing saga of Sakurai's object (V4334 Sgr): dust production and helium line emission

We report further UKIRT spectroscopic observations of Sakurai's object (V4334 Sgr) made in 1999 April/May in the 1-4.75 µm range, and find that the emission is dominated by amorphous carbon at T[subscript d] ~ 600. The estimated maximum grain size is 0.6 µm, and the mass lower limit is 1.7 ± 0.2 x 10[superscript -8] M[subscript ¤] to 8.9 ± 0.6 x 10[superscript -7] M[subscript ¤] for distances of 1.1-8 kpc. For 3.8 kpc the mass is 2.0 ± 0.1 x 10[superscript -7] M[subscript ¤]. We also report strong He i emission at 1.083 µm, in contrast to the strong absorption in this line in 1998. We conclude that the excitation is collisional, and is probably caused by a wind, consistent with the P Cygni profile observed by Eyres et al. in 1998

The February 1999 superoutburst of the SU UMa-type dwarf nova CG CMa

The original article can be found at : http://www.konkoly.hu/cgi-bin/IBVS4759--Copyright Konkoly ObservatoryPeer reviewe

Photometric data and analysis of the light curve of the W UMa-variable ST Ind

Photoelectric observations of the W UMa variable ST Ind are analyzed which were obtained at the European Southern Observatory in the course of a program to monitor light curve fluctuations. Photometric and geometric elements of ST Ind are derived. The observations show the presence of a periodic fluctuation in certain parts of the light curve which may be explained by the precessional motion of the rotation axis of the brighter component. © 1989 Kluwer Academic Publishers

Photometric data and analysis of the light curve of the W UMa-variable ST Ind

Photoelectric observations of the W UMa variable ST Ind are analyzed which were obtained at the European Southern Observatory in the course of a program to monitor light curve fluctuations. Photometric and geometric elements of ST Ind are derived. The observations show the presence of a periodic fluctuation in certain parts of the light curve which may be explained by the precessional motion of the rotation axis of the brighter component. © 1989 Kluwer Academic Publishers

X-ray and optical-to-infrared follow-up observations of the transient X-ray burster SAX J1810.8-2609

We have performed a ROSAT follow-up observation of the X-ray transient SAX J1810.8-2609 on March 24, 1998 and detected a bright X-ray source (named RX J1810.7-2609) which was not detected during the ROSAT all-sky survey in September 1990. Optical-to-infrared follow-up observations of the 10 arcsec radius ROSAT HRI X-ray error box revealed one variable object (R = 19.5+/-0.5 on 13 March, R>21.5 on 27 Aug 1998) which we tentatively propose as the optical/IR counterpart of RX J1810.7-2609 = SAX J1810.8-2609.Comment: 4 pages with mn.sty; MNRAS (accept.) also available from http://www.aip.de/~jcg/publis.htm