Abstract
The B star HD192273 was tentatively identified1 as an extremeultraviolet (EUV) source. Photometry2 and photographic spectra of this star show that the optical and EUV fluxes fit a model with Te = 27,000 K and log g = 4.8, values reasonably close to those of a normal B2 V star. However, if HD 192273 is such a normal main-sequence star, its distance D is ∼4 kpc, difficult to reconcile with the low line-of-sight column density (<1018 cm−2 over the 4-kpc path), the low radial velocity (−24 km s−1), and the high distance (∼2 kpc) out of the galactic plane. Instead, we suggest that this object is an analogue of HZ22, an evolved, low-mass component of a binary3, where the spectroscopic log g is consistent with a relatively small radius (0.1–1 R⊙ and a small distance D of 100–200 pc. Such a suggestion can explain both the low H I column density and the small radial velocity.
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Shipman, H., Wegner, G. The high-latitude EUV source HD192273 as a low-mass binary. Nature 281, 126–127 (1979). https://doi.org/10.1038/281126a0
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DOI: https://doi.org/10.1038/281126a0
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