1RXS J174320.1-042953: another polar with a red-shifted absorption component in emission line wings
Abstract
We present the results of a spectroscopic and multi-band photometric study of the magnetic cataclysmic variable 1RXS J174320.1-042953. Multi-band photometry confirms a periodic modulation with an orbital period of Porb=0.0864 ± 0.0001 days. Using the estimated secondary mass of ∼0.15 M⊙ and, the X-ray-based white dwarf mass of ∼0.75 M⊙, we obtain values of q∼0.2 and a system inclination of 47∘±10∘. The optical spectra of 1RXS J174320.1-042953 are dominated by strong, complex, asymmetric, and highly variable single-peaked emission lines of the Balmer series, \ion{He}{i}, and \ion{He}{ii}, which are characteristic of polar-type magnetic cataclysmic variables. Doppler tomography reveals no evidence of a Keplerian accretion disc, supporting the classification of the system as a polar. The Hβ and \ion{He}{ii} emission lines can be decomposed into at least two distinct components. The low-velocity components have semi-amplitudes of approximately 170 km s−1 (Hβ) and 147 km s−1 (\ion{He}{ii}), while the high-velocity components reach about 317 km s−1 and 460 km s−1, respectively. The low-velocity component is likely associated with the irradiated side of the secondary star facing the white dwarf and/or the vicinity of the L1 point, whereas the high-velocity component is related to the accretion-stream structure. A redshifted absorption component in the emission-line wings is detected at orbital phases near ϕ≈ 0.0, reaching velocities up to ∼1400 km s−1 and likely produced by accretion-stream material crossing the line of sight.
Related
- Mathematical Framework for the Effects of Sample Absorption on Raman Intensity for Quantification and Detection Thresholds of Minerals in Two-Component Geological Mixtures.
- H I Absorbers as Beacons of Hidden Structure at z ∼ 3: Multi-Component, Metal-Rich Absorption System near a Protocluster
- Wave Emission and Absorption in a Near-Sun Proton-Cyclotron Wave Storm
- Predicting High-Energy neutrino emission from X-ray absorption in CSM-interacting SNe
- EMU detection of mysterious multiple component radio-continuum emission from nearby spiral Seyfert I type galaxy ‘Sand-timer’ (NGC 7213)
BibTeX
@misc{gonzalezbuitrago20261rxs,
title = {{1RXS J174320.1-042953: another polar with a red-shifted absorption component in emission line wings}},
author = {Diego H. González-Buitrago and Ma. T. García-Díaz and Sergey Zharikov and Gagik Tovmassian and A. Castro and E. J. Kotze and Yair Krongold and C. A. Negrete},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.01032},
eprint = {2610.01032},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.01032},
}
RIS
TY - UNPB
TI - 1RXS J174320.1-042953: another polar with a red-shifted absorption component in emission line wings
AU - Diego H. González-Buitrago
AU - Ma. T. García-Díaz
AU - Sergey Zharikov
AU - Gagik Tovmassian
AU - A. Castro
AU - E. J. Kotze
AU - Yair Krongold
AU - C. A. Negrete
PY - 2026
DA - 2026/10/01
PB - arXiv
DO - 10.48550/arxiv.2610.01032
UR - https://arxiv.org/abs/2610.01032
AB - We present the results of a spectroscopic and multi-band photometric study of the magnetic cataclysmic variable 1RXS J174320.1-042953. Multi-band photometry confirms a periodic modulation with an orbital period of P_orb=0.0864 ± 0.0001 days. Using the estimated secondary mass of ∼0.15 M_⊙ and, the X-ray-based white dwarf mass of ∼0.75 M_⊙, we obtain values of q∼0.2 and a system inclination of 47^∘±10^∘. The optical spectra of 1RXS J174320.1-042953 are dominated by strong, complex, asymmetric, and highly variable single-peaked emission lines of the Balmer series, \ion{He}{i}, and \ion{He}{ii}, which are characteristic of polar-type magnetic cataclysmic variables. Doppler tomography reveals no evidence of a Keplerian accretion disc, supporting the classification of the system as a polar. The Hβ and \ion{He}{ii} emission lines can be decomposed into at least two distinct components. The low-velocity components have semi-amplitudes of approximately 170 km s^−1 (Hβ) and 147 km s^−1 (\ion{He}{ii}), while the high-velocity components reach about 317 km s^−1 and 460 km s^−1, respectively. The low-velocity component is likely associated with the irradiated side of the secondary star facing the white dwarf and/or the vicinity of the L_1 point, whereas the high-velocity component is related to the accretion-stream structure. A redshifted absorption component in the emission-line wings is detected at orbital phases near ϕ≈ 0.0, reaching velocities up to ∼1400 km s^−1 and likely produced by accretion-stream material crossing the line of sight.
ER -