[vsnet-alert 20780] Re: OV Boo outburst
isogai at kusastro.kyoto-u.ac.jp
Wed Mar 15 03:42:10 JST 2017
This is an additional information.
OV Boo is also known as SDSS J1507+52. In order to explain why the orbital period
is below the period minimum although the object has WZ Sge-like properties,
Patterson et al. (2008) proposed that the secondary of OV Boo might be a
Population II (metal-poor) star. (Because Pop. II star is smaller than normal stars.)
However, the spectroscopic study is insufficient, and the population has not
If this outburst is "metal-poor outburst", the behavior might be different from
the ordinary DNe outburst.
On 2017年03月15日 02:51, Keisuke Isogai wrote:
> OV Boo has ultra-short period of 0.046 d, and the period is below the period minimum.
> By the spectroscopic study, Patterson et al. (2008) suggested that OV Boo is a member
> of WZ Sge stars, but the object had shown no outbursts.
> This outburst is very likely to be a WZ Sge-like superoutburst. Thus time-series
> observations are strongly encouraged.
> On 2017年03月15日 01:42, Seiichi Yoshida wrote:
>> Dear colleagues,
>> I am Seiichi Yoshida working on the MISAO Project.
>> Masaru Mukai, Kagoshima, Japan, reported that OV Boo
>> (R.A. 15 07 22.35, Decl. +52 30 39.8) is bright as 11.4 mag on
>> Mar. 14.63 (UT), using Nikon 105-mm lens + CCD (STL6303E) + IR-cut
>> The VSX data shows it is a CV+EA+ZZ/GWLIB type with a range of
>> 18.0-20.6 mag.
>> Best regards,
>> Seiichi Yoshida
>> comet at aerith.net
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