English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We report the first radial velocity spectroscopic study of the eclipsingperiod bouncer SDSS J105754.25+275947.5. Together with eclipse light curvemodeling, we redetermined the system parameters and studied the accretion diskstructure. We confirm that the system contains a white dwarf with$M_{\mathrm{WD}}=0.83(3) M_\odot$ and an effective temperature of 11,500(400)K.The mass of the secondary is $M_2 = 0.056 M_\odot$ with an effectivetemperature of T$_2$=2,100K or below. The system inclination is $i=84.3(6)$.The data is in good agreement with our determination of $K_1$ = 33(4) kms$^{-1}$. We estimate the mass transfer rate as $\dot{M}=$1.9(2)$\times10^{-11} M_\odot yr^{-1}$. Based on an analysis of the SDSS and OSIRIS spectra,we conclude that the optical continuum is formed predominantly by the radiationfrom the white dwarf. The contribution of the accretion disk is low andoriginates from the outer part of the disk. The Balmer emission lines areformed in a plasma with $\log$ $N_0$ = 12.7 [cm$^{-1}$] and a kinetictemperature of T$\sim$10,000K. The size of the disk, where the emission linesare formed, expands up to $R_\mathrm{d,out}=0.29 R_\odot$. The inner part ofthe emission line forming region goes down to $R_\mathrm{d,in}\approx 2R_\mathrm{WD}$ . The Doppler tomography and trailed spectra show the presenceof a hot spot and a clumpy structure in the disk, with variable intensity alongthe disk position angle. There is an extended region at the side opposite thehot spot with two bright clumps caused more probably by non-Keplerian motionthere.

The period bouncer system SDSS J105754.25+275947.5: first radial velocity study