We have analyzed phase-resolved photometric and spectroscopic observations of the eclipsing polar SDSS J002637.06+242915.6.The light curve has a M-shaped bright phase that was reproduced using a simple model of an acc...We have analyzed phase-resolved photometric and spectroscopic observations of the eclipsing polar SDSS J002637.06+242915.6.The light curve has a M-shaped bright phase that was reproduced using a simple model of an accreting magnetic white dwarf.The hydrogen emission lines exhibit a narrow component formed on the irradiated hemisphere of the donor.The Doppler tomography revealed differences in the positions of emission regions of hydrogen and HeⅡλ4686 lines.The spectra exhibit a Zeeman absorption triplet of the Hαline,formed in the cold halo around the accretion spot at a magnetic field strength of B=15.1±1.3 MG.The spectra of the bright phase have a red cyclotron continuum,whose orbital variability has been interpreted within a simple model of an accretion spot.The modeling of the cyclotron continuum constrains the white dwarf's magnetic field to B_(cyc)■45 MG.The analysis of the eclipse light curve and the radial velocities of the irradiated hemisphere yielded estimates for the orbital inclination■,the mass ratio 0.23≤q≤0.43,and the white dwarf mass 0.72≥M_(1)/M_(⊙)≥0.42.展开更多
美国斯隆数字化巡天(SDSS)类星体光谱中存在明显的大气天光谱线，这对类星体光谱的分析尤其是吸收线的证认造成较大干扰.以SDSS D R 1 0 的光谱为样本，对光谱中的天光线进行研究，给出了[01]姿5577魡残差的分布.发现光谱[01]姿5577魡...美国斯隆数字化巡天(SDSS)类星体光谱中存在明显的大气天光谱线，这对类星体光谱的分析尤其是吸收线的证认造成较大干扰.以SDSS D R 1 0 的光谱为样本，对光谱中的天光线进行研究，给出了[01]姿5577魡残差的分布.发现光谱[01]姿5577魡残差处于5572.5586魡的范围内.这一结果为证认吸收线的工作提供参考，同时将有利于改进主成分分析减天光方法.展开更多
基金supported by the Ministry of Science and Higher Education of the Russian Federation。
文摘We have analyzed phase-resolved photometric and spectroscopic observations of the eclipsing polar SDSS J002637.06+242915.6.The light curve has a M-shaped bright phase that was reproduced using a simple model of an accreting magnetic white dwarf.The hydrogen emission lines exhibit a narrow component formed on the irradiated hemisphere of the donor.The Doppler tomography revealed differences in the positions of emission regions of hydrogen and HeⅡλ4686 lines.The spectra exhibit a Zeeman absorption triplet of the Hαline,formed in the cold halo around the accretion spot at a magnetic field strength of B=15.1±1.3 MG.The spectra of the bright phase have a red cyclotron continuum,whose orbital variability has been interpreted within a simple model of an accretion spot.The modeling of the cyclotron continuum constrains the white dwarf's magnetic field to B_(cyc)■45 MG.The analysis of the eclipse light curve and the radial velocities of the irradiated hemisphere yielded estimates for the orbital inclination■,the mass ratio 0.23≤q≤0.43,and the white dwarf mass 0.72≥M_(1)/M_(⊙)≥0.42.
文摘美国斯隆数字化巡天(SDSS)类星体光谱中存在明显的大气天光谱线，这对类星体光谱的分析尤其是吸收线的证认造成较大干扰.以SDSS D R 1 0 的光谱为样本，对光谱中的天光线进行研究，给出了[01]姿5577魡残差的分布.发现光谱[01]姿5577魡残差处于5572.5586魡的范围内.这一结果为证认吸收线的工作提供参考，同时将有利于改进主成分分析减天光方法.
