An international team of astronomers has conducted a comprehensive spectroscopic and photometric study of an eclipsing binary pulsar known as AI Hya. The results of the study published on January 11 on the arXiv prepress server, providing important insights into the nature of this system.
Ecliptic binaries (EBs) are systems that display regular light variations due to a star passing directly in front of its companion. In EBs, the orbital plane of the two stars is approximately in the observer’s line of sight such that the components undergo mutual eclipses. These systems can provide a direct measurement of the mass, radius and effective temperature of stars.
Pulsars are variables in which changes in brightness are due to changes in the area and temperature of the star’s surface layers. Some types of pulsars, such as Beta Cepheids, Delta Scuti stars, and Gamma Doradus stars, are also found in EBs.
Located around 2000 light years Far away, AI Hya is an eclipsing binary with a Delta Scuti component consisting of star F2m and F0V. she has eccentric orbit The orbital period is about 8.29 days. Since no high-resolution spectra of AI Hya have been performed yet, a group of astronomers led by Filiz Kahraman Alicavos of Çanakkale Onsekiz Mart University in Turkey conducted a detailed optical and spectral analysis of this system in order to reveal what it really is. nature.
In this study, we present a detailed analysis of the discrete pulsed binary system and the AI Hya binary eclipse studied by two independent groups In different ways. We performed a spectral survey to estimate orbital parameters via radial velocity measurements and atmospheric parameters for each binary component using composite and/or unentangled spectra,” the researchers wrote in the paper.
The analyzed data was collected using NASA’s Transiting Exoplanet Survey Satellite (TESS) and several ground-based observatories. The study found that the brightest component of AI Hya is a massive star (2.09 solar masses), a cool, chemically normal star, about 3.86 times more massive than the Sun, while the hottest component is a slightly metal-rich object with a radius of about 2.76 solar radii and a mass of about 1.95 solar masses.
initial orbital From AI Hya was determined to be 8.34 days, while the initial orbital eccentricity was estimated to be 0.24. The age of the system has been calculated to be around 850-860 million years.
The astronomers confirmed that with regard to the evolutionary status of AI Hya, both components are within the Delta Scuti instability band. According to the exact age, they assume that this system is at an important evolutionary stage in terms of binary evolution.
Rapidly evolving mega ingredient The process of mass transfer to the least massive will begin about 20 million years from now. This situation can cause significant differences in the oscillation properties,” the paper’s authors predicted.
Kahraman Alikavouss et al., Comprehensive spectroscopic and photometric study of the eclipsing binary pulsar AI Hya, arXiv (2023). doi: 10.48550/arxiv.2301.04409
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