000005507 001__ 5507
000005507 005__ 20230120145830.0
000005507 0247_ $$2DOI$$a10.3847/1538-4357/ac45fb
000005507 037__ $$aSCART-2021-0159
000005507 100__ $$aPanchal, A.
000005507 245__ $$aLong-term photometric and low-resolution spectroscopic analysis of five contact binaries
000005507 260__ $$c2022
000005507 520__ $$aA photometric and spectroscopic investigation is performed on five W Ursae Majoris eclipsing binaries (EWs) J015818.6+260247 (hereinafter as J0158b), J073248.4+405538 (hereinafter as J0732), J101330.8+494846 (hereinafter as J1013), J132439.8+130747 (hereinafter as J1324) and J152450.7+245943 (hereinafter as J1524). The photometric data are collected with the help of the 1.3 m Devasthal Fast Optical Telescope (DFOT), the 1.04 m Sampurnanand Telescope (ST) and the TESS space mission. The low-resolution spectra of the 4 m Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) are used for spectroscopic analysis. The orbital period change of these systems is determined using our and previously available photometric data from different surveys. The orbital period of J1013 and J1524 is changing with a rate of −2.552(±0.249) × 10 −7 days yr −1 and −6.792(±0.952) × 10^−8 days yr^−1, respectively, while others do not show any orbital period change. The orbital period change of J1013 and J1524 corresponds to a mass transfer rate of 2.199 × 10^−7 M_⊙ yr^−1 and 6.151 × 10^−8 M_⊙ yr^−1 from the primary to the secondary component in these systems. It is likely that angular momentum loss via magnetic braking may also be responsible for the observed orbital period change in the case of J1524. All systems have a mass-ratio lower than 0.5, except J0158b with a mass-ratio of 0.71. All the systems are shallow type contact binaries. The J0158b and J1524 are A-subtype while others are W-subtype. The H α emission line region is compared with template spectra prepared using two inactive stars with the help of STARMOD program. The J0158, J1324 and J1524 systems show excess emission in the residual spectra after subtraction of the template.
000005507 594__ $$aNO
000005507 6531_ $$abinaries: close
000005507 6531_ $$atechniques: photometric
000005507 6531_ $$atechniques: spectroscopic
000005507 6531_ $$abinaries : eclipsing
000005507 6531_ $$abinaries : contact
000005507 6531_ $$afundamental : parameters
000005507 700__ $$aJoshi, Y.
000005507 700__ $$aDe Cat, P.
000005507 700__ $$aTiwari, S.
000005507 773__ $$c1--18 (id. 12)$$pThe Astrophysial Journal$$v927$$y2022
000005507 85642 $$ahttps://ui.adsabs.harvard.edu/abs/2022ApJ...927...12P/abstract
000005507 8560_ $$fpeter.decat@observatoire.be
000005507 8564_ $$s6048780$$uhttp://publi2-as.oma.be/record/5507/files/Panchal2022_ApJ927_12.pdf
000005507 8564_ $$s3672$$uhttp://publi2-as.oma.be/record/5507/files/Panchal2022_ApJ927_12.gif?subformat=icon$$xicon
000005507 8564_ $$s6517$$uhttp://publi2-as.oma.be/record/5507/files/Panchal2022_ApJ927_12.jpg?subformat=icon-180$$xicon-180
000005507 905__ $$apublished in
000005507 980__ $$aREFERD