| Autor: |
Israel, G. L., Hummel, W., Covino, S., Campana, S., Appenzeller, I., Gässler, W., Mantel, K.-H., Marconi, G., Mauche, C. W., Munari, U., Negueruela, I., Nicklas, H., Rupprecht, G., Smart, R. L., Stahl, O., Stella, L., Israel, G. L., Hummel, W., Covino, S., Campana, S., Appenzeller, I., Gässler, W., Mantel, K.-H., Marconi, G., Mauche, C. W., Munari, U., Negueruela, I., Nicklas, H., Rupprecht, G., Smart, R. L., Stahl, O., Stella, L. |
| Zdroj: |
Astronomy and Astrophysics; April 2002, Vol. 386 Issue: 1 pL13-L17, 5p |
| Abstrakt: |
We carried out optical observations of the field of the X–ray pulsator RX J0806.3+1527. A blue $V =$21.1 star was found to be the only object consistent with the X–ray position. VLT FORS spectra revealed a blue continuum with no intrinsic absorption lines. Broad ($v \sim$1500 km s-1), low equivalent width (~–1 $\div$–6 Å) emission lines from the HeII Pickering series were clearly detected. B, Vand Rtime–resolved photometry revealed the presence of ~15% pulsations at the ~321 s X–ray period, confirming the identification. These findings, together with the period stability and absence of any additional modulation in the 1 min$ - $5 hr period range, argue in favour of the orbital interpretation of the 321 s pulsations. The most likely scenario is thus that RX J0806.3+1527 is a double degenerate system of the AM CVn class. This would make RX J0806.3+1527 the shortest orbital period binary currently known and one of the best candidates for gravitational wave detection. |
| Databáze: |
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