The Fe Line Flux Ratio as a Diagnostic of the Maximum Temperature and the White Dwarf Mass of Cataclysmic Variables

Xu, Xiaojie; Yu, Zhuo-li; Li, Xiangdong

doi:10.3847/1538-4357/ab1fe1

Cited by 16 publications

(37 citation statements)

References 38 publications

(60 reference statements)

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“…The PSR model produces results consistent (within 90 per cent uncertainties) with those of Xu et al (2019), though we note that the PSR model results in smaller uncertainties. The completion of the Legacy survey, which was still in progress at the time of publication of Xu et al (2019), adds 13 more mCVs to the NuSTAR archive. In future studies of the Legacy data, we will be able to examine if this consistency between the two methodologies holds for all mCVs.…”

Section: Comparisons With Masses Derived From the Iron Line Complexsupporting

confidence: 66%

“…Lower Panel: Histogram of WD masses from post-common-envelope binaries (grey) and a subset of that sample considered to be representative of progenitors of current CVs ('pre-CVs; ' Zorotovic et al 2011, hatched). 2019, and this work) with those derived using the Fe line ratio method on the same NuSTAR data (combined with Suzaku data, Xu et al 2019) in Fig. 5.…”

Section: Comparisons With Masses Derived From the Iron Line Complexmentioning

confidence: 64%

“…This is achieved by measuring the intensity ratio of the H-like (7.0 keV) and He-like (6.7 keV) components of the Fe complex, which is correlated with the temperature of the PSR. Using the NuSTAR observations of mCVs available at the time (some of which are Legacy targets), Xu et al (2019) applied a similar methodology to derive M WD for a number of systems. We directly compare the masses derived using the PSR model (Suleimanov et al Suleimanov et al 2019, hatched) and the non-magnetic CVs (grey; Zorotovic et al 2011).…”

Section: Comparisons With Masses Derived From the Iron Line Complexmentioning

confidence: 99%

“…The Legacy data set that resulted in this work is extensive, and PSR modelling of the >20 keV spectra is just one of the analysis approaches we can take. Xu et al (2019) showed, with a small number of NuSTAR spectra, that there is a wealth of information embedded within the Fe line complex that can lead to an independent derivation of PSR temperature and therefore mass. In addition, a study of the full 3-78 keV spectra will allow us to conduct an in-depth analysis of reflection and partial covering in mCVs, allowing estimates of the shock height, as well as an alternative spectral fitting method to measure M WD .…”

Section: Future Workmentioning

confidence: 99%

“…X-ray spectroscopy provides a method of measuring WD mass independent of radial velocity studies, which are often dominated by uncertainties in binary inclination (Suleimanov, Revnivtsev & Ritter 2005;Yuasa et al 2010;Suleimanov, Doroshenko & Werner 2019). An alternative Xray spectroscopic method compares the fluxes from Fe-K lines of different ionization states to measure the post-shock temperature (Fujimoto & Ishida 1997;Ezuka & Ishida 1999;Xu, Yu & Li 2019).…”

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confidence: 99%

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Measuring the masses of magnetic white dwarfs: a NuSTAR legacy survey

Shaw

Heinke

Mukai

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The hard X-ray spectrum of magnetic cataclysmic variables can be modelled to provide a measurement of white dwarf mass. This method is complementary to radial velocity measurements, which depend on the (typically rather uncertain) binary inclination. Here we present results from a Legacy Survey of 19 magnetic cataclysmic variables with NuSTAR. We fit accretion column models to their 20–78 keV spectra and derive the white dwarf masses, finding a weighted average $\bar{M}_{\rm WD}=0.77\pm 0.02$M⊙, with a standard deviation σ = 0.10 M⊙, when we include the masses derived from previous NuSTAR observations of seven additional magnetic cataclysmic variables. We find that the mass distribution of accreting magnetic white dwarfs is consistent with that of white dwarfs in non-magnetic cataclysmic variables. Both peak at a higher mass than the distributions of isolated white dwarfs and post-common-envelope binaries. We speculate as to why this might be the case, proposing that consequential angular momentum losses may play a role in accreting magnetic white dwarfs and/or that our knowledge of how the white dwarf mass changes over accretion–nova cycles may also be incomplete.

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Section: Comparisons With Masses Derived From the Iron Line Complexsupporting

confidence: 66%

Section: Comparisons With Masses Derived From the Iron Line Complexmentioning

confidence: 64%

Section: Comparisons With Masses Derived From the Iron Line Complexmentioning

confidence: 99%

Section: Future Workmentioning

confidence: 99%

mentioning

confidence: 99%

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Measuring the masses of magnetic white dwarfs: a NuSTAR legacy survey

Shaw

Heinke

Mukai

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The mass of the white dwarf in YY Dra (=DO Dra): Dynamical measurement and comparative study with X-ray estimates

Álvarez-Hernández,

Torres,

Shahbaz

et al. 2024

A&A

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We present a dynamical study of the intermediate polar cataclysmic variable based on time-series observations in the $K$ band, where the donor star is known to be the major flux contributor. We covered the $3.97$-h orbital cycle with 44 spectra taken between $2020$ and $2022$ and two epochs of photometry observed in 2021 March and May. One of the light curves was simultaneously obtained with spectroscopy to better account for the effects of irradiation of the donor star and the presence of accretion light. From the spectroscopy, we derived the radial velocity curve of the donor star metallic absorption lines, constrained its spectral type to M0.5--M3.5 with no measurable changes in the effective temperature between the irradiated and non-irradiated hemispheres of the star, and measured its projected rotational velocity $v_ rot i = 103 km s $. Through simultaneous modelling of the radial velocity and light curves, we derived values for the radial velocity semi-amplitude of the donor star, $K_2 = 188^ the donor to white dwarf mass ratio, $q=M_2/M_1 = 0.62 0.02$, and the orbital inclination circ circ circ $. These binary parameters yield dynamical masses of $M_ M odot $ and $M_2 = 0.62^ M odot $ ($68$ per cent confidence level). As found for the intermediate polars GK Per and XY Ari, the white dwarf dynamical mass in YY Dra significantly differs from several estimates obtained by modelling the X-ray spectral continuum.

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A Study on White Dwarf Masses in Cataclysmic Variables Based on XMM-Newton and Suzaku Observations

Yu¹,

Xu²,

Li³

2022

Res. Astron. Astrophys.

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The distribution of the mass of white dwarfs (WDs) is one of the fundamental questions in the field of cataclysmic variables (CVs). In this work, we make a systematical investigation on the WD masses in two subclass of CVs: intermediate polars (IPs) and non- magnetic CVs in the Solar vicinity based on the flux ratios of FeXXVI-Lyα to FeXXV-Heα emission lines (I7.0/I6.7) from archival XMM–Newton and Suzaku observations. We firstly verify the (semi-empirical) relations between I7.0/I6.7, the maximum emission temperature (Tmax) and the WD mass (MWD) with the mkcflow model based on the apec description and the latest AtomDB. We then introduce a new spectral model to measure MWD directly based on the above relations. Comparison shows that the derived MWD are consistent with dynamically measured ones. At last, we obtain the average WD masses of 58 CVs (including 36 IPs and 22 non-magnetic CVs), which is the largest X-ray selected sample. The average WD masses are < MWD,IP >= 0.81 ± 0.21M⊙ and < MWD,DN >= 0.81 ± 0.21M⊙ for IPs and non-magnetic CVs, respectively. These results are consistent with previous works.

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The Fe Line Flux Ratio as a Diagnostic of the Maximum Temperature and the White Dwarf Mass of Cataclysmic Variables

Cited by 16 publications

References 38 publications

Measuring the masses of magnetic white dwarfs: a NuSTAR legacy survey

Measuring the masses of magnetic white dwarfs: a NuSTAR legacy survey

The mass of the white dwarf in YY Dra (=DO Dra): Dynamical measurement and comparative study with X-ray estimates

A Study on White Dwarf Masses in Cataclysmic Variables Based on XMM-Newton and Suzaku Observations

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