رؤى - Astronomy and Astrophysics - # Pulsating Stars in Detached Eclipsing Binaries

Detailed Analysis of Five Candidate Delta Scuti-type Pulsators in Detached Eclipsing Binary Systems

Q: How do the pulsation properties of these stars compare to isolated delta Scuti variables, and what insights can be gained about the effects of binarity on stellar oscillations?

The pulsation properties of the candidate δ Scuti-type pulsators in detached eclipsing binaries (DEBs) exhibit both similarities and differences when compared to isolated δ Scuti variables. Isolated δ Scuti stars typically display pressure mode oscillations with periods ranging from approximately 18 minutes to 8 hours and amplitudes below 0.1 magnitudes in the V-band. In contrast, the pulsators within DEBs, such as those analyzed in this study, may experience additional complexities due to their binary nature. One significant insight gained from studying these pulsators is the impact of tidal interactions on their oscillation properties. For instance, in TIC 81702112, the observed amplitude modulation of pulsation frequencies over the orbital phase suggests that tidal forces are influencing the pulsation characteristics. This modulation can lead to variations in the pulsation amplitudes and frequencies, which are not typically observed in isolated δ Scuti stars. Furthermore, the presence of a companion star can induce changes in the pulsation modes, potentially leading to tidally induced pulsations or altered mode stability. Overall, the study of pulsating stars in DEBs provides a unique opportunity to explore the interplay between binarity and stellar oscillations, offering insights into how tidal forces and the gravitational environment of a binary system can modify the pulsation behavior of stars.

Q: What are the potential limitations of the spectroscopic analysis, especially for the high-rotation systems, and how could these be addressed in future studies?

The spectroscopic analysis of high-rotation systems, such as those in the sample studied, presents several limitations. One major challenge is the broadening of spectral lines due to rapid rotation, which can obscure the details necessary for accurate parameter determination. High rotational velocities can lead to significant line blending, making it difficult to distinguish between the contributions of individual components in a binary system. This blending can result in inaccurate estimates of effective temperature (T_eff), surface gravity (log g), and metallicity, as seen in TIC 165459595, where the high rotation and low signal-to-noise ratio (S/N) hindered precise measurements. To address these limitations in future studies, several approaches could be implemented. First, obtaining higher-resolution spectra would help resolve blended lines and improve the accuracy of parameter estimates. Utilizing advanced spectrographs with higher spectral resolution, such as those available at larger telescopes, could enhance the quality of the data. Additionally, employing techniques such as spectral disentangling and broadening function analysis can help isolate the contributions of individual stars in a binary system, allowing for more accurate modeling of their spectra. Moreover, incorporating a larger sample of observations over different orbital phases could provide a more comprehensive view of the system's dynamics and improve the reliability of the derived parameters. Finally, utilizing synthetic spectral fitting with improved models that account for rapid rotation and its effects on line profiles could enhance the accuracy of the analysis.

Q: Could the observed amplitude modulation in TIC 81702112 be used to infer details about the internal structure and tidal interactions in this eccentric binary system?

Yes, the observed amplitude modulation in TIC 81702112 can indeed be used to infer details about the internal structure and tidal interactions within this eccentric binary system. The variability in the amplitude of pulsation frequencies over the orbital phase suggests that tidal forces are playing a significant role in shaping the pulsation behavior of the stars. This modulation can provide insights into the distribution of mass and the internal structure of the pulsating star, as well as the effects of tidal interactions between the two components. In eccentric binaries, the varying gravitational influence during different phases of the orbit can lead to changes in the pulsation modes. For instance, the tidal forces exerted by the companion star can induce additional oscillation modes or alter the stability of existing modes. By analyzing the amplitude modulation, researchers can gain insights into the degree of tidal coupling between the stars, which can be indicative of their internal structure, such as the presence of a convective core or the stratification of different layers within the star. Furthermore, the amplitude modulation can also provide information about the synchronization of rotation and orbital motion. By comparing the observed modulation patterns with theoretical models of tidal interactions, it is possible to infer the efficiency of tidal dissipation and the extent to which the stars have synchronized their rotation with the orbital period. This information can contribute to a better understanding of the evolutionary history of the system and the processes governing the interaction between the stars in a binary system.

المفاهيم الأساسية

Comprehensive photometric and spectroscopic analysis of five candidate delta Scuti-type pulsators in detached eclipsing binary systems to obtain precise stellar parameters and study the pulsation properties.

الملخص

The authors performed a detailed analysis of five candidate delta Scuti-type pulsators in detached eclipsing binary (DEB) systems. The key highlights are:

Photometric and spectroscopic data, including high-precision TESS light curves and high-resolution spectra, were used to model the binary systems and obtain precise stellar parameters.
Light curve and radial velocity modeling was done to estimate the absolute stellar parameters, while detailed spectroscopic analysis provided the global metallicity and temperatures.
Frequency power spectra were obtained from the residuals after binary modeling to study the pulsation properties of the stars.
For TIC 81702112, the authors report variable amplitude of the dominant pulsation frequency over the orbital phase, likely due to tidal effects.
The precise stellar parameters obtained were used to determine the age of the systems by comparing with theoretical isochrones.
The analysis provides strong constraints on the physical properties of these pulsating stars in DEBs, which can serve as anchors for future asteroseismic studies.

تخصيص الملخص

إعادة الكتابة بالذكاء الاصطناعي

إنشاء الاستشهادات

ترجمة المصدر

إلى لغة أخرى

إنشاء خريطة ذهنية

من محتوى المصدر

زيارة المصدر

arxiv.org

الإحصائيات

"The masses and radii of the components are constrained to a high accuracy, which helps us constrain the age of the systems."
"For TIC 81702112, we report tidal effects causing amplitude variation in the oscillation frequencies over the orbital phase."

اقتباسات

"Pulsating stars in eclipsing binaries (EBs) provide an excellent opportunity to obtain precise, model-independent stellar parameters for studying these oscillations in detail."
"Accurate modelling of observed pulsations thus provides us with a tool to probe the internal structure of stars."

الرؤى الأساسية المستخلصة من

Comprehensive study of five candidate delta Scuti-type pulsators in detached eclipsing binaries

by T. P... في arxiv.org 10-02-2024

https://arxiv.org/pdf/2410.00590.pdf

Comprehensive study of five candidate delta Scuti-type pulsators in detached eclipsing binaries

استفسارات أعمق

How do the pulsation properties of these stars compare to isolated delta Scuti variables, and what insights can be gained about the effects of binarity on stellar oscillations?

The pulsation properties of the candidate δ Scuti-type pulsators in detached eclipsing binaries (DEBs) exhibit both similarities and differences when compared to isolated δ Scuti variables. Isolated δ Scuti stars typically display pressure mode oscillations with periods ranging from approximately 18 minutes to 8 hours and amplitudes below 0.1 magnitudes in the V-band. In contrast, the pulsators within DEBs, such as those analyzed in this study, may experience additional complexities due to their binary nature.
One significant insight gained from studying these pulsators is the impact of tidal interactions on their oscillation properties. For instance, in TIC 81702112, the observed amplitude modulation of pulsation frequencies over the orbital phase suggests that tidal forces are influencing the pulsation characteristics. This modulation can lead to variations in the pulsation amplitudes and frequencies, which are not typically observed in isolated δ Scuti stars. Furthermore, the presence of a companion star can induce changes in the pulsation modes, potentially leading to tidally induced pulsations or altered mode stability.
Overall, the study of pulsating stars in DEBs provides a unique opportunity to explore the interplay between binarity and stellar oscillations, offering insights into how tidal forces and the gravitational environment of a binary system can modify the pulsation behavior of stars.

What are the potential limitations of the spectroscopic analysis, especially for the high-rotation systems, and how could these be addressed in future studies?

The spectroscopic analysis of high-rotation systems, such as those in the sample studied, presents several limitations. One major challenge is the broadening of spectral lines due to rapid rotation, which can obscure the details necessary for accurate parameter determination. High rotational velocities can lead to significant line blending, making it difficult to distinguish between the contributions of individual components in a binary system. This blending can result in inaccurate estimates of effective temperature (T_eff), surface gravity (log g), and metallicity, as seen in TIC 165459595, where the high rotation and low signal-to-noise ratio (S/N) hindered precise measurements.
To address these limitations in future studies, several approaches could be implemented. First, obtaining higher-resolution spectra would help resolve blended lines and improve the accuracy of parameter estimates. Utilizing advanced spectrographs with higher spectral resolution, such as those available at larger telescopes, could enhance the quality of the data. Additionally, employing techniques such as spectral disentangling and broadening function analysis can help isolate the contributions of individual stars in a binary system, allowing for more accurate modeling of their spectra.
Moreover, incorporating a larger sample of observations over different orbital phases could provide a more comprehensive view of the system's dynamics and improve the reliability of the derived parameters. Finally, utilizing synthetic spectral fitting with improved models that account for rapid rotation and its effects on line profiles could enhance the accuracy of the analysis.

Could the observed amplitude modulation in TIC 81702112 be used to infer details about the internal structure and tidal interactions in this eccentric binary system?

Yes, the observed amplitude modulation in TIC 81702112 can indeed be used to infer details about the internal structure and tidal interactions within this eccentric binary system. The variability in the amplitude of pulsation frequencies over the orbital phase suggests that tidal forces are playing a significant role in shaping the pulsation behavior of the stars. This modulation can provide insights into the distribution of mass and the internal structure of the pulsating star, as well as the effects of tidal interactions between the two components.
In eccentric binaries, the varying gravitational influence during different phases of the orbit can lead to changes in the pulsation modes. For instance, the tidal forces exerted by the companion star can induce additional oscillation modes or alter the stability of existing modes. By analyzing the amplitude modulation, researchers can gain insights into the degree of tidal coupling between the stars, which can be indicative of their internal structure, such as the presence of a convective core or the stratification of different layers within the star.
Furthermore, the amplitude modulation can also provide information about the synchronization of rotation and orbital motion. By comparing the observed modulation patterns with theoretical models of tidal interactions, it is possible to infer the efficiency of tidal dissipation and the extent to which the stars have synchronized their rotation with the orbital period. This information can contribute to a better understanding of the evolutionary history of the system and the processes governing the interaction between the stars in a binary system.