43 research outputs found
OT J002656.6+284933 (CSS101212:002657+284933): An SU UMa-Type Dwarf Nova with Longest Superhump Period
We observed the 2016 outburst of OT J002656.6+284933
(CSS101212:002657+284933) and found that it has the longest recorded
[0.13225(1) d in average] superhumps among SU UMa-type dwarf novae. The object
is the third known SU UMa-type dwarf nova above the period gap. The outburst,
however, was unlike ordinary long-period SU UMa-type dwarf novae in that it
showed two post-outburst rebrightenings. It showed superhump evolution similar
to short-period SU UMa-type dwarf novae. We could constrain the mass ratio to
less than 0.15 (most likely between 0.10 and 0.15) by using superhump periods
in the early and post-superoutburst stages. These results suggest the
possibility that OT J002656.6+284933 has an anomalously undermassive secondary
and it should have passed a different evolutionary track from the standard one.Comment: 6 pages, 3 figures, accepted for publication in PASJ (Letters), Note
added in proof has been added. Supplementary Information (si.pdf) is
available in the source fil
Periodicities in the high-mass X-ray binary system RXJ0146.9+6121/LSI+61 235
The high-mass X-ray binary RX J0146.9+6121, with optical counterpart LS I+61°235 (V831 Cas), is an intriguing system on the outskirts of the open cluster NGC 663. It contains the slowest Be type X-ray pulsar known with a pulse period of around 1400 s and, primarily from the study of variation in the emission line profile of Hα, it is known to have a Be decretion disc with a one-armed density wave period of approximately 1240 d. Here we present the results of an extensive photometric campaign, supplemented with optical spectroscopy, aimed at measuring short time-scale periodicities. We find three significant periodicities in the photometric data at, in order of statistical significance, 0.34, 0.67 and 0.10 d. We give arguments to support the interpretation that the 0.34 and 0.10 d periods could be due to stellar oscillations of the B-type primary star and that the 0.67 d period is the spin period of the Be star with a spin axis inclination of 23+10−8 degrees. We measured a systemic velocity of −37.0 ± 4.3 km s−1 confirming that LS I+61°235 has a high probability of membership in the young cluster NGC 663 from which the system's age can be estimated as 20–25 Myr. From archival RXTE All Sky Monitor (ASM) data we further find ‘super’ X-ray outbursts roughly every 450 d. If these super outbursts are caused by the alignment of the compact star with the one-armed decretion disc enhancement, then the orbital period is approximately 330 d