VLBI detection of the AE Aqr twin, LAMOST J024048.51+195226.9

Abstract

LAMOST J024048.51+195226.9 (J0240+1952) was recently identified as the second AE Aquarii (AE Aqr)-type cataclysmic variable, possessing the fastest known rotating white dwarf. We performed a Very Long Baseline Interferometry (VLBI) observation of J0240+1952 utilizing the European VLBI Network at 1.7\,GHz, to obtain the first view of the radio morphology on mas scale. Our high-resolution VLBI image clearly shows that the radio emission is compact on mas scale ($\lesssim 2$\,AU), with no evidence for a radio jet or extended emission. The compact radio source has an average flux density of $\sim 0.37$\,mJy, and its brightness temperature is given at $\gtrsim 2.3\times 10^7$\,K, confirming a non-thermal origin. The emission exhibits irregular variations on a time-scale of tens of minutes, similar to the radio flares seen in AE Aqr. The measured VLBI position of J0240+1952 is consistent with that derived from \textit{Gaia}. Our results favour the model in which the radio emission is attributed to a superposition of synchrotron radiation from expanding magnetized blobs of this system.

References in corpus (11)

• Gaia Data Release 3: Summary of the content and survey properties
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• The SFXC software correlator for Very Long Baseline Interferometry: Algorithms and Implementation
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• Precise radio astrometry and new developments for the next generation of instruments
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• VLA Observations of the AE Aqr-type Cataclysmic Variable LAMOST J024048.51+195226.9

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