Possible Density Determination of the Nebular Component of Cataclysmic Variables with the N III 4641/4635 Line Ratio

Bohigas, J.; Tijerina, Eduardo Pérez; Machorro, R.

doi:10.1017/s0252921100153035

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“…The emission line ratio N III 4641/4635 has been used as a diagnostic for electron density in hot plasmas produced in pulsed laser deposition experiments for thin film depositions (Bohigas, Pérez-Tijerina & Machorro 2004). These authors determined population levels in a 10.000 K plasma considering radiative decay and collisional excitation and de-excitation.…”

Section: The λλ 4640-4650 Emission and Possible X-ray Excitationmentioning

confidence: 99%

The remarkable properties of the symbiotic star AE Circinus

Mennickent

Greiner

Arenas

et al. 2007

Monthly Notices of the Royal Astronomical Society

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We present new optical spectroscopy and photometry, 2MASS infrared observations and 24 years of combined AAVSO and AFOEV photometry of the symbiotic star candidate \ae. The long-term light curve is characterized by outbursts lasting several years and having a slow decline of $\sim 2 \times 10^{-4}$ mag/day. The whole range of variability of the star in the $V$ band is about 4 magnitudes. The periodogram of the photometric data reveals strong signals at $\sim$ 342 and 171 days. The presence of the emission feature at $\lambda$ 6830 \AA at minimum and the detection of absorption lines of a $\sim$ K5 type star confirm the symbiotic classification and suggest that AE Cir is a new member of the small group of s-type yellow symbiotic stars. We estimate a distance of 9.4 kpc. Our spectrum taken at the high state shows a much flatter spectral energy distribution, the disappearance of the $\lambda$ 6830 \AA emission feature and the weakness of the He II 4686 emission relative to the Balmer emission lines. Our observations indicate the presence of emission line flickering in time scales of minutes in 2001. The peculiar character of \ae is revealed in the visibility of the secondary star at the high and low state, the light curve resembling a dwarf nova superoutburst and the relatively short low states. The data are hard to reconciliate with standard models for symbiotic star outbursts.Comment: accepted for publication in MNRAS, 7 figure

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Section: The λλ 4640-4650 Emission and Possible X-ray Excitationmentioning

confidence: 99%