Comprehensive Catalogue of δ Scuti Pulsators in Binary Systems as of 2024

แนวคิดหลัก

The updated catalogue of δ Scuti pulsators in binary systems contains over 1000 such objects, providing detailed statistical properties, correlations, and evolutionary diagrams of these stars.

บทคัดย่อ

This work presents the largest catalogue of δ Scuti (DS) pulsators in binary systems, containing 1,048 DS in 1,043 systems as of 2024. The sample is divided based on the Roche geometry of the binary systems to investigate any systematic differences in the pulsators' evolution due to the proximity of the companion star.
The key highlights and insights from the analysis include:

Demographics and statistics: The catalogue contains detailed information on the variability types, Roche geometries, and physical properties (mass, radius, temperature, pulsation frequency) of the DS pulsators. Only about 10% of the sample have accurately determined absolute parameters.

Correlations: The well-established correlation between the orbital (Porb) and pulsation (Ppul) periods is updated, with a limit of 12.5-13 days in Porb beyond which they are uncorrelated. The correlation between the evolutionary status (log g) and Ppul also shows differences between DS in short-period detached/semidetached systems and those in long-period detached systems.

Evolutionary diagrams: The majority of binary DS are Main-Sequence stars located within the classical instability strip, in contrast with single DS stars. Only a few cases are found below the Zero-Age or beyond the Terminal-Age Main-Sequence.

Future prospects: With the upcoming data releases from Gaia, TESS, and PLATO, the sample of binary DS with well-known physical properties is expected to increase significantly, allowing for more detailed studies on the influence of binarity on the pulsational behavior of these stars.

สถิติ

The DS in binary systems have masses between 1.25-2.9 M⊙ and radii between 1.3-4.4 R⊙.
The dominant pulsation frequencies of DS in detached systems range between 5-10 d^-1, while those in semidetached binaries have a peak between 15-20 d^-1.

คำพูด

"The vast majority of binary DS are Main-Sequence stars in contrast with the single DS."
"There is correlation between evolutionary stage and the dominant frequency of the binary DS that is similar between the members of short-period detached and semidetached binaries but totally different from that of single DS."

ข้อมูลเชิงลึกที่สำคัญจาก

The catalogue of $\delta$ Sct pulsators in binary systems in 2024

by Alexios Liak... ที่ arxiv.org 10-02-2024

https://arxiv.org/pdf/2410.00763.pdf

สอบถามเพิ่มเติม

How do the pulsational properties of binary DS differ from those of single DS stars, and what are the underlying physical mechanisms responsible for these differences?

The pulsational properties of binary δ Scuti (DS) stars exhibit notable differences compared to their single counterparts, primarily influenced by the presence of a companion star. In binary systems, the dominant pulsation frequencies of DS stars tend to be higher, particularly in semidetached systems, where the pulsation frequency distribution peaks between 15-20 d⁻¹. In contrast, detached binary DS stars show a distribution peak within the range of 5-10 d⁻¹. This variation can be attributed to the effects of binarity on stellar structure and evolution.
The underlying physical mechanisms responsible for these differences include the influence of tidal interactions and mass transfer processes. In semidetached systems, the gravitational pull from the companion star can enhance pulsation amplitudes and frequencies due to the increased effective temperature and altered stellar structure. Additionally, the kappa mechanism, which drives pulsations in DS stars, may be affected by the presence of a companion, leading to changes in the opacity and energy transport processes within the pulsating star. The interaction between the pulsational modes and the binary environment can also result in longer preservation of pulsations in binary DS stars compared to single DS stars, as indicated by the observed differences in the log g-Ppul correlation.

What are the potential implications of the observed differences in the Porb-Ppul and log g-Ppul correlations between binary DS in different Roche geometries on our understanding of stellar evolution and pulsation excitation mechanisms?

The observed differences in the Porb-Ppul and log g-Ppul correlations among binary DS stars in various Roche geometries have significant implications for our understanding of stellar evolution and pulsation excitation mechanisms. The established correlation between orbital period (Porb) and pulsation period (Ppul) suggests that the proximity of the companion star influences the pulsational behavior of the DS component. For instance, the limit of 12.5-13 days in Porb, beyond which Porb and Ppul become uncorrelated, indicates a threshold where the effects of binarity on pulsation excitation diminish. This finding can inform models of stellar evolution by highlighting the role of binary interactions in shaping the evolutionary paths of pulsating stars.
Furthermore, the log g-Ppul correlation reveals that binary DS stars exhibit different evolutionary stages compared to single DS stars. The similarity in the correlation for short-period detached and semidetached systems suggests that these stars may share common evolutionary traits influenced by their binary nature. In contrast, the lack of correlation for detached systems with Porb > 12.5 d implies that these stars may evolve independently of their companions, leading to distinct pulsational characteristics. Understanding these correlations can enhance our knowledge of how binarity affects stellar structure, pulsation modes, and the overall evolutionary processes of DS stars.

Given the expected increase in the sample of binary DS with well-determined physical properties, how can future studies leverage this information to provide new insights into the interplay between binarity, stellar structure, and pulsational behavior?

The anticipated increase in the sample of binary DS stars with well-determined physical properties presents a unique opportunity for future studies to deepen our understanding of the interplay between binarity, stellar structure, and pulsational behavior. As more accurate measurements of parameters such as mass, radius, and temperature become available, researchers can conduct comprehensive analyses of the pulsational characteristics of these stars in relation to their binary configurations.
Future studies can leverage this expanded dataset to refine models of stellar evolution, particularly in the context of binary interactions. By examining the correlations between Porb, Ppul, and log g across a larger and more diverse sample, researchers can identify trends and anomalies that may reveal new insights into the mechanisms driving pulsation excitation and the effects of binarity on stellar evolution. Additionally, the availability of radial velocity measurements from missions like Gaia will enhance the accuracy of mass determinations, allowing for more robust comparisons between binary and single DS stars.
Moreover, the exploration of hybrid pulsational behavior in binary systems, where DS stars exhibit characteristics of both δ Scuti and γ Doradus stars, can provide valuable information about the conditions under which different pulsation modes are excited. This could lead to a better understanding of the physical processes governing pulsations in various stellar environments. Overall, the integration of new data and advanced modeling techniques will facilitate a more comprehensive understanding of the complex relationships between binarity, stellar structure, and pulsational behavior in δ Scuti stars.