LkH$alpha$ 225 (V1318 Cyg) South in Outburst. (arXiv:2108.05406v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Hillenbrand_L/0/1/0/all/0/1">Lynne A. Hillenbrand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Isaacson_H/0/1/0/all/0/1">Howard Isaacson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_A/0/1/0/all/0/1">Antonio C. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Connelley_M/0/1/0/all/0/1">Michael Connelley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reipurth_B/0/1/0/all/0/1">Bo Reipurth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuhn_M/0/1/0/all/0/1">Michael A. Kuhn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beck_T/0/1/0/all/0/1">Tracy Beck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_D/0/1/0/all/0/1">Diego Rodriguez Perez</a>

Magakian et al. (2019) called attention to the current bright state of LkHa
225 South, which over the past two decades has changed from $>20^m$ to $<13^m$.
We present recent optical photometric monitoring that shows colorless,
non-sinusoidal, periodic brightness variations. The oscillations occur every 43
days, and have amplitude $sim$0.7 mag with some variation among cycles. We
also present new flux-calibrated optical and near-infrared spectroscopy, which
we model in terms of a keplerian disk. Additional high dispersion spectra
demonstrate the similarity of the absorption line pattern to some categories of
“mixed temperature” accretion outburst objects. At blue wavelengths, LkHa 225
South has a pure absorption spectrum and is a good spectral match to the FU Ori
stars V1515 Cyg and V1057 Cyg. At red optical and infrared wavelengths,
however, the spectrum is more similar to Gaia 19ajj, showing emission in TiO,
CO, and metals. Sr II lines indicate a low surface gravity atmosphere. There
are also signatures of a strong wind/outflow. LkHa 225 South was moderately
bright in early 1950’s as well as in late 1980’s, with evidence for deep fades
during intervening epochs. The body of evidence suggests that LkHa225 South is
another case of a source with episodically enhanced accretion that causes
brightening by orders of magnitude, and development of a hot absorption
spectrum and warm wind. It is similar to Gaia 19ajj, but also reminiscent in
its long brightening time and brightness oscillation near peak, to the embedded
sources L1634 IRS7 and ESO Ha 99.

Magakian et al. (2019) called attention to the current bright state of LkHa
225 South, which over the past two decades has changed from $>20^m$ to $<13^m$.
We present recent optical photometric monitoring that shows colorless,
non-sinusoidal, periodic brightness variations. The oscillations occur every 43
days, and have amplitude $sim$0.7 mag with some variation among cycles. We
also present new flux-calibrated optical and near-infrared spectroscopy, which
we model in terms of a keplerian disk. Additional high dispersion spectra
demonstrate the similarity of the absorption line pattern to some categories of
“mixed temperature” accretion outburst objects. At blue wavelengths, LkHa 225
South has a pure absorption spectrum and is a good spectral match to the FU Ori
stars V1515 Cyg and V1057 Cyg. At red optical and infrared wavelengths,
however, the spectrum is more similar to Gaia 19ajj, showing emission in TiO,
CO, and metals. Sr II lines indicate a low surface gravity atmosphere. There
are also signatures of a strong wind/outflow. LkHa 225 South was moderately
bright in early 1950’s as well as in late 1980’s, with evidence for deep fades
during intervening epochs. The body of evidence suggests that LkHa225 South is
another case of a source with episodically enhanced accretion that causes
brightening by orders of magnitude, and development of a hot absorption
spectrum and warm wind. It is similar to Gaia 19ajj, but also reminiscent in
its long brightening time and brightness oscillation near peak, to the embedded
sources L1634 IRS7 and ESO Ha 99.

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