Spectroscopic and Photometric Study of the new $\delta$ Scuti Star ASAS J063309+1810.8

TL;DR

This study characterizes the new $\,\delta$ Scuti star ASAS J063309+1810.8 through spectroscopic and photometric observations, revealing its pulsation properties, physical parameters, and evolutionary status.

Contribution

It provides the first detailed spectroscopic and photometric analysis of the new $\,\delta$ Scuti star, including updated pulsation frequencies, physical parameters, and evolutionary insights.

Findings

Identified the star as a low-amplitude $\,\delta$ Scuti with a 102.6 min period.

Determined fundamental parameters: Teff=7125K, log g=4.0, M=1.595 M_sun.

Measured pulsation frequencies and provided an updated ephemeris.

Abstract

We present BVR observations and low-resolution spectra collected by the Kottamia Astronomical Observatory 1.88 m telescope (KAO) for the new pulsating star ASAS J063309+1810.8 (hereafter it will be called ASAS06+18). The photometric analysis revealed that the star is a $\delta$ Scuti star with low amplitude (a=0.054-0.099 in V mag.) and a short period (102.604 min). Fourier analysis of the light curves reveals the fundamental mode with two harmonics. The photometric analysis yielded a new value of the updated frequency of 13.0035232 cd-1 with an amplitude of 49.93 mmag at phases 0.326 and S/N 21.75 and to two frequencies (20.2099237cd-1, 5.9130945cd-1). Given the available data, 37 new times of maximum light are presented, and an updated ephemeris for the star and its O-C data. Assuming its period decreases and changes smoothly, a new value of (1/P)dP/dt is determined. We calculated the effective temperature and surface gravity as Teff=7125+- 250 K and log g=4.0+-0.2 dex from model atmosphere analysis of the star's spectra at different phases. The bolometric magnitude Mbol=2.798 (0.016), radius R=1.577(0.077) R_sun, luminosity L=5.714(1.066) L_sun, the mass is M=1.595 M_sun and pulsation constant Q=0{\^m}.0338(0.0003). The star's locations in the evolutionary mass-luminosity and mass-radius relationships are discussed.