Taurus star cluster
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The Taurus Star Cluster: Insights from Recent Research
Multiplicity and Clustering in Taurus Star Cluster
The Taurus star-forming region is a prime example of a quiescent star-forming area, providing critical insights into the star formation process. Recent studies have identified local overdense stellar structures, termed Nested Elementary Structures (NESTs), which are crucial for understanding the spatial distribution of stars in Taurus. These NESTs are densely packed regions containing between four and 23 stars, with surface densities reaching up to 2500 stars per square parsec. They are primarily aligned along the principal gas filaments and represent the preferred sites of star formation in Taurus .
Stellar Membership and Initial Mass Function (IMF)
High-precision astrometry from the Gaia mission has significantly refined the census of members in the Taurus star-forming region. This refined census has provided better constraints on the distribution of ages and the initial mass function (IMF) in Taurus. Contrary to previous beliefs, there is no population of older stars (around 10 Myr) associated with the Taurus clouds. The IMF across the region shows little variation, indicating a consistent star formation process across different stellar densities .
Substructure and Star Formation History
The Taurus-Auriga complex exhibits a complex star formation history with observable imprints on its spatial, kinematic, and temporal structure. The region is substructured into clustered groups near the clouds and sparse groups spread throughout the area. The sparse groups are generally older, suggesting a sequential star formation process triggered from behind the clouds. This complex history indicates at least two epochs of star formation, featuring both clustered and distributed modes .
Structure and Kinematics
The structure and kinematics of the Taurus star-forming region reveal significant depth effects, with molecular clouds located at varying distances. For instance, the L 1495 molecular cloud is at approximately 130 parsecs, while connected filamentary structures are around 160 parsecs away. The region shows no clear evidence of expansion or contraction but does exhibit signs of potential global rotation. The tight coupling between the stars and the underlying molecular gas is evident from the minimal difference in their radial velocities .
Age Distribution and Kinematic Groups
Using Gaia data, researchers have divided the Taurus members into 13 groups with distinct kinematics. Most groups have median ages of around 1-3 Myr, while neighboring associations have ages ranging from 13 to 56 Myr. This age distribution supports the idea of a sequential star formation process within the region. Additionally, the presence of circumstellar disks among some members indicates ongoing star formation activities .
Chemical Composition
The Taurus-Auriga association has a solar metallicity, with a mean [Fe/H] value of -0.01 ± 0.05. This uniformity in metallicity among members suggests that the region's stars formed from a chemically homogeneous environment. The lack of metal-rich members aligns with observations in other star-forming regions, reinforcing the idea that older, metal-rich stars form closer to the Galactic center and migrate outward .
Mass Segregation
The Taurus association exhibits inverse mass segregation, with the most massive stars being less centrally concentrated compared to lower-mass stars. This contrasts with the strong mass segregation observed in denser clusters like Orion. Brown dwarfs in Taurus are not mass segregated, although some low-mass stars show signs of segregation .
Rotation Rates and Variability
Analysis of K2 light curves reveals that a significant portion of Taurus members exhibit periodic rotation. The distribution of rotation rates is similar to other young clusters, with slower rotators among early M spectral types and faster rotation towards both earlier FGK and later M types. Stars with circumstellar disks tend to rotate slower, and the overall amplitude of light curves decreases with age .
New Member Surveys
Surveys using data from the Sloan Digital Sky Survey (SDSS) and Spitzer Space Telescope have identified new members of the Taurus star-forming region. These surveys have refined the census of members and provided additional insights into the region's initial mass function. The updated census shows a surplus of solar-mass stars, although less pronounced than previously thought Luhman2016Luhman2009.
Conclusion
The Taurus star cluster continues to be a rich field of study, offering valuable insights into the star formation process. From the identification of dense stellar structures to the refined census of members and the complex star formation history, recent research has significantly advanced our understanding of this prototypical low-mass star-forming region. The findings underscore the importance of high-precision astrometry and multi-wavelength surveys in unraveling the intricacies of star formation.
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