activity
20182021
most citedStellar and accretion disk parameters of the close binary HD 50526

5 citations · 6 across the 2 of their papers we have counts for

collaborators

6 papers

astro-ph.SR20211 cited

Fundamental parameters of the eclipsing binary DD CMa and evidence for mass exchange

J. A. Rosales, R. E. Mennickent, G. Djurašević +5

We present a detailed photometric and spectroscopic analysis of DD CMa, based on published survey photometry and new spectroscopic data. We find an improved orbital period of $P_\m…

astro-ph.SR20215 cited

Stellar and accretion disk parameters of the close binary HD 50526

J. A. Rosales, R. E. Mennickent, G. Djurašević +5

We present a photometric and spectroscopic study of HD 50526, an ellipsoidal binary member of the group Double Periodic Variable stars. Performing data-mining in photometric survey…

astro-ph.SR2019

New Double Periodic Variable Stars in the ASAS-SN Catalog

J. A. Rosales, R. E. Mennickent

We report the discovery of 3 new Double Periodic Variables based on the analysis of ASAS-SN light curves: GSD J11630570-510306, V593 Sco and TYC 6939-678-1. These systems have orbi…

astro-ph.SR2018

Evolutionary process of the interacting binary V495 Centauri

J. A. Rosales, R. E. Mennickent, D. R. G. Schleicher +1

We present a simple model for the Double Periodic Variable (DPV) V495 Cen, which evolves as a binary system of intermediate mass, where the gainer cannot accrete at high rate, limi…

astro-ph.SR2018

Dynamo effect in the double periodic variable DQ Velorum

R. I. San Martín-Pérez, D. R. G. Schleicher, R. E. Mennickent +1

DQ Velorum is a galactic double periodic variable (DPV), this system is a semi-detached binary comprised of a B-type gainer and an A-type donor star plus an extended accretion disc…

astro-ph.SR2018

TYC 5353-1137-1: an enigmatic Double Periodic Variable of semiregular amplitude

J. A. Rosales, R. E Mennickent

We have performed a new search for DPVs of short period in the ASAS catalog (Pojmanski, G., 1997), focusing on those stars with orbital periods between 2 to 3 days which also show…