scholarly journals Cloud Computing Bayesian Approach to Study Effects of Binary Stars on Ages of Star Clusters

2021 ◽  
Vol 1927 (1) ◽  
pp. 012022
Author(s):  
Jing Chen ◽  
Su Zhang ◽  
Zhongmu Li
Keyword(s):  
Cloud Computing ◽  
Bayesian Approach ◽  
Binary Stars ◽  
Star Clusters

scholarly journals Modeling of Integrated Spectral Energy Distributions of Stellar Populations with Various Binary Fractions

2021 ◽  
Vol 2068 (1) ◽  
pp. 012048
Author(s):  
Zhongmu Li ◽  
Chen Yan
Keyword(s):  
Binary Stars ◽  
Star Clusters ◽  
Stellar Populations ◽  
Spectral Studies ◽  
Spectral Energy ◽  
Spectral Energy Distributions ◽  
Energy Distributions ◽  
Spectral Fitting ◽  
The Universe

Abstract Binary stars are common in the universe, but binary fractions are various in different star clusters and galaxies. Studies have shown that binary fraction affects the integrated spectral energy distributions obviously, in particular in the UV band. It affects spectral fitting of many star clusters and galaxies significantly. However, previous works usually take a fixed binary fraction, i.e., 0.5, and this is far from getting accurate results. Therefore, it is important to model the integrated spectral energy distributions of stellar populations with various binary fractions. This work presents a modeling of spectral energy distributions of simple stellar populations with binary fractions of 0.3, 0.7, and 1.0. The results are useful for different kinds of spectral studies.

3. Stars

2016 ◽  
pp. 22-49
Author(s):  
James Binney
Keyword(s):  
Star Formation ◽  
20Th Century ◽  
Binary Stars ◽  
Star Clusters ◽  
Solar Neutrinos ◽  
Interstellar Gas ◽  
Stellar Seismology ◽  
Stellar Masses ◽  
Century Science ◽  
The Universe

Most of what we know about the Universe has been gleaned from the study of stars, and a major achievement of 20th-century science was to understand how stars work and their lifecycles from birth to death. ‘Stars’ describes this lifecycle beginning with star formation when a cloud of interstellar gas suffers a runaway of its central density. It then considers nuclear fusion, key stellar masses, and life after the main sequence when the star burns its core helium. The surfaces of stars are described along with stellar coronae and exploding stars—both core-collapse and deflagration supernovae. Finally, globular star clusters, solar neutrinos, stellar seismology, and binary stars are discussed.

scholarly journals The Formation and Evolution of LMC Globular Clusters: The Database

1999 ◽  
Vol 190 ◽  
pp. 460-461 ◽  
Author(s):  
S. F. Beaulieu ◽  
R. Elson ◽  
G. Gilmore ◽  
R. A. Johnson ◽  
N. Tanvir ◽  
...  
Keyword(s):  
Binary Stars ◽  
Globular Clusters ◽  
Star Clusters ◽  
Data Set ◽  
Luminosity Functions ◽  
Formation And Evolution ◽  
Mass Segregation ◽  
Large Cycle

We present details of the database from a large Cycle 7 HST project to study the formation and evolution of rich star clusters in the LMC (see Elson et al., this volume). Our data set, which includes NICMOS, WFPC2 and STIS images of 8 clusters, will enable us to derive deep luminosity functions for the clusters and to investigate the universality of the stellar IMF. We will look for age spreads in the youngest clusters, quantify the population of binary stars in the cores of the clusters and at the half-mass radii, and follow the development of mass segregation.

scholarly journals THE CONTRIBUTIONS OF INTERACTIVE BINARY STARS TO DOUBLE MAIN-SEQUENCE TURNOFFS AND DUAL RED CLUMP OF INTERMEDIATE-AGE STAR CLUSTERS

2011 ◽  
Vol 731 (2) ◽  
pp. L37 ◽  
Author(s):  
Wuming Yang ◽  
Xiangcun Meng ◽  
Shaolan Bi ◽  
Zhijia Tian ◽  
Tanda Li ◽  
...  
Keyword(s):  
Binary Stars ◽  
Main Sequence ◽  
Star Clusters ◽  
Red Clump

scholarly journals Isolated Binaries and Triples in N-body Systems

1995 ◽  
Vol 164 ◽  
pp. 372-372
Author(s):  
J. Anosova ◽  
L. Kiseleva
Keyword(s):  
Globular Cluster ◽  
Binary Stars ◽  
Star Clusters ◽  
Dynamical Evolution ◽  
Time Interval ◽  
Galactic Field ◽  
Multiple Stars ◽  
Binary And Multiple Stars ◽  
Marked Tendency ◽  
Triple Stars

Stars show a marked tendency to form the systems of different multiplicity starting from the smallest systems as binary and triple stars up to clusters with a significantly larger number of objects (N ~ 107 for globular cluster s). Different investigators have used different methods of binary stars identificati on but modern observations give a frequency of binary and multiple stars in the Galactic field up to 70% Binary and multiple stars are also often present within star clusters. It is therefore very important to be able to identify such systems as rather isolated substructures in which the dynamical evolution is not significantly affected by other stars (at least, during some considerab le time interval).

scholarly journals The black hole retention fraction in star clusters

2018 ◽  
Vol 617 ◽  
pp. A69 ◽  
Author(s):  
Václav Pavlík ◽  
Tereza Jeřábková ◽  
Pavel Kroupa ◽  
Holger Baumgardt
Keyword(s):  
Binary Stars ◽  
Globular Clusters ◽  
Dwarf Galaxies ◽  
Star Clusters ◽  
One Dimensional ◽  
Mass Segregation ◽  
The One ◽  
Good Agreement ◽  
Effective Distribution ◽  
Retention Fraction

Context. Recent research has been constraining the retention fraction of black holes (BHs) in globular clusters by comparing the degree of mass segregation with N-body simulations. They are consistent with an upper limit of the retention fraction being 50% or less. Aims. In this work, we focus on direct simulations of the dynamics of BHs in star clusters. We aim to constrain the effective distribution of natal kicks that BHs receive during supernova (SN) explosions and to estimate the BH retention fraction.Methods. We used the collisional N-body code nbody6 to measure the retention fraction of BHs for a given set of parameters, which are: the initial mass of a star cluster, the initial half-mass radius, and σBH, which sets the effective Maxwellian BH velocity kick distribution. We compare these direct N-body models with our analytic estimates and newest observational constraints. Results. The numerical simulations show that for the one-dimensional velocity kick dispersion σBH < 50 km s−1, clusters with radii of 2 pc and that are initially more massive than 5 × 103 M⊙ retain more than 20% of BHs within their half-mass radii. Our simple analytic model yields a number of retained BHs that is in good agreement with the N-body models. Furthermore, the analytic estimates show that ultra-compact dwarf galaxies should have retained more than 80% of their BHs for σBH ≤ 190 km s−1. Although our models do not contain primordial binaries, in the most compact clusters with 103 stars, we have found evidence of delayed SN explosions producing a surplus of BHs compared to the IMF due to dynamically formed binary stars. These cases do not occur in the more populous or expanded clusters.

scholarly journals Three-Body Problem and Multiple Stellar Systems

2004 ◽  
Vol 191 ◽  
pp. 146-151
Author(s):  
M. Valtonen
Keyword(s):  
Binary Stars ◽  
Body Problem ◽  
Star Clusters ◽  
Point Of View ◽  
Stellar Systems ◽  
Three Body Problem ◽  
Single Star ◽  
Triple Systems ◽  
Break Up ◽  
Three Body

AbstractThree-body processes go on in star clusters where binary stars meet single stars and frequently form temporary triple systems. The triples are typically unstable and break up into a new binary and a single star. Also a simple scattering of a single star from a binary may take place. Both processes can be handled by the statistical theories of three-body break-up and scattering. Here we apply the theory to binary stars, assuming that binaries have been involved in the three-body process. The distributions of binary periods, eccentricities and mass ratios are discussed from this point of view and compared with observational samples.

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