The nature of the close magnetic white dwarf + probable brown dwarf binary SDSS J121209.31+013627.7*
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منابع مشابه
The nature of the close magnetic white dwarf + probable brown dwarf binary SDSS
Optical time series photometry of the short period magnetic white dwarf + probable brown dwarf binary SDSS J121209.31 + 013627.7 reveals pulse-like variability in all bands from i to u, increasing towards bluer wavelengths and peaking at u. These modulations are most likely due to a self-eclipsing accretion hot spot on the white dwarf, rotating into view every 88.43 minutes. This period is comm...
متن کاملThe nature of the close magnetic white dwarf + probable brown dwarf binary
Optical time series photometry of the short period magnetic white dwarf + probable brown dwarf binary SDSS J121209.31 + 013627.7 reveals pulse-like variability in all bands from i to u, peaking at u. These modulations are most likely due to a self-eclipsing accretion hot spot on the white dwarf, rotating into view every 88.43 minutes. This period is commensurate with the radial velocity period ...
متن کاملThe nature of the close magnetic white dwarf + probable brown dwarf binary SDSS J 121209 . 31 + 013627 . 7 ⋆
Optical time series photometry of the short period magnetic white dwarf + probable brown dwarf binary SDSS J121209.31 + 013627.7 reveals pulse-like variability in all bands from i to u, increasing towards bluer wavelengths and peaking at u. These modulations are most likely due to a self-eclipsing accretion hot spot on the white dwarf, rotating into view every 88.43 minutes. This period is comm...
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A near-infrared excess is detected at the white dwarf PHL 5038 in UKIDSS photometry, consistent with the presence of a cool, substellar companion. We have obtained Hand K-grism spectra and images of PHL 5038 using NIRI on Gemini North. The target is spatially and spectrally resolved into two components; an 8000 K DA white dwarf, and a likely L8 brown dwarf companion, separated by 0.94 ′′. The s...
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We present high-speed, three-colour photometry of the eclipsing cataclysmic variable SDSS J150722.30+523039.8 (hereafter SDSS J1507). This system has an orbital period of 66.61 minutes, placing it below the observed “period minimum” for cataclysmic variables. We determine the system parameters via a parameterised model of the eclipse fitted to the observed lightcurve by χ minimisation. We obtai...
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ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 2006
ISSN: 1365-2966,0035-8711
DOI: 10.1111/j.1365-2966.2006.11030.x