Showing 1-25 of 12,382 resultsfor "Index Terms":Star Model
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Uncover: Toward Interpretable Models for Detecting New Star Cluster Members
Sebastian Ratzenböck;Verena Obermüller;Torsten Möller;João Alves;Immanuel M. Bomze
In this design study, we present Uncover, an interactive tool aimed at astronomers to find previously unidentified member stars in stellar clusters. We contribute data and task abstraction in the domain of astronomy and provide an approach for the non-trivial challenge of finding a suitable hyper-parameter set for highly flexible novelty detection models. We achieve this by substituting the tediou...Show More
New PARSEC evolutionary tracks of massive stars at low metallicity: testing canonical stellar evolution in nearby star-forming dwarf galaxies
We extend the PARSEC library of stellar evolutionary tracks by computing new models of massive stars, from 14 to 350 M⊙. The input physics is the same used in the PARSEC V1.1 version, but for the mass-loss rate from considering the most recent updates in the literature. We focus on low metallicity, Z = 0.001 and Z = 0.004, for which the metal-poor dwarf irregular star-forming galaxies, Sextans A, ...Show More
The Red MSX Source survey: critical tests of accretion models for the formation of massive stars
There is currently no accepted theoretical framework for the formation of the most massive stars, and the manner in which protostars continue to accrete and grow in mass beyond ∼10 M⊙ is still a controversial topic. In this study we use several prescriptions of stellar accretion and a description of the Galactic gas distribution to simulate the luminosities and spatial distribution of massive prot...Show More
The theoretical mass-magnitude relation of low-mass stars and its metallicity dependence
We investigate the dependence of theoretically generated mass-absolute magnitude relations on stellar models. Using up-to-date physics we compute models of stars in the mass range 0.1 < m ≤ 1 M⊙. We compare the solar-metallicity models with our older models and also with recent models computed by others. We further compare them with an empirical mass-absolute magnitude relation that best fits the ...Show More
Research on the Influencing Factors of the P/E Ratio of Listed Companies on STAR Market
2023 5th International Conference on Decision Science & Management (ICDSM)
Year: 2023 | Conference Paper |
STAR Market was announced in 2018 as a new board separate from the existing main board market. And then opened in June 2019, with the official opening of the market in the following July. Since the establishment of STAR Market is not long and the data of several companies have not yet been disclosed, the data are selected to take quarterly as the time span, and the data of seventy companies listed...Show More
Effect of dynamical interactions on integrated properties of globular clusters
Globular clusters (GCs) are generally treated as natural validators of simple stellar population (SSP) models. However, there are still some differences between real GCs and SSPs. In this work, we use a direct N-body simulation code NBODY6 to study the influences of dynamical interactions, metallicity and primordial binaries on Milky Way GCs’ integrated properties. Our models start with N = 100 00...Show More
Quasi-periodic oscillations in low-mass X-ray binaries and constraints on the equation of state of neutron star matter
Recently discovered quasi-periodic oscillations in the X-ray brightness of low-mass X-ray binaries are used to derive constraints on the mass of the neutron star component and the equation of state of neutron star matter. The observations are compared with models of rapidly rotating neutron stars which are calculated by means of an exact numerical method in full relativity. For the equations of st...Show More
The standard model of low-mass star formation applied to massive stars: multiwavelength modelling of IRAS 20126+4104
In order to investigate whether massive stars form similarly to their low-mass counterparts, we have used the standard envelope plus disc geometry successfully applied to low-mass protostars to model the near-IR to submillimetre spectral energy distribution (SED) and several mid-IR images of the embedded massive star IRAS 20126+4104. We have used a Monte Carlo radiative transfer dust code to model...Show More
Formation and evolution of binary neutron stars: mergers and their host galaxies
In this paper, we investigate the properties of binary neutron stars (BNSs) and their mergers by combining population synthesis models for binary stellar evolution (BSE) with cosmological galaxy formation and evolution models. We obtain constraints on BSE model parameters by using the observed Galactic BNSs and local BNS merger rate density (R0) inferred from gravitational wave (GW) observations, ...Show More
Spatial statistics in star-forming regions: is star formation driven by column density alone?
Star formation is known to occur more readily where more raw materials are available. This is often expressed by a ‘Kennicutt–Schmidt’ relation where the surface density of young stellar objects (YSOs) is proportional to column density to some power, μ. The aim of this work was to determine if column density alone is sufficient to explain the locations of Class 0/I YSOs within Serpens South, Serpe...Show More
The influence of the environment on the spin evolution of low-mass stars – I. External photoevaporation of circumstellar discs
Massive stars are strong sources of far-ultraviolet radiation that can be hostile to the evolution of protoplanetary discs, driving mass-loss by external photoevaporation and shortening disc-dissipation time-scales. Their effect may also reduce the time-scale of angular momentum exchanges between the disc and host star during the early pre-main-sequence phase. To improve our understanding of the e...Show More
The asteroseismological potential of the pulsating DB white dwarf stars CBS 114 and PG 1456+103
We have acquired 65 h of single-site time-resolved CCD photometry of the pulsating DB white dwarf star (DBV) CBS 114 and 62 h of two-site high-speed CCD photometry of another DBV, PG 1456+103. The pulsation spectrum of PG 1456+103 is complicated and variable on time-scales of approximately 1 week and could only partly be deciphered with our measurements. The modes of CBS 114 are more stable in tim...Show More
Deep Learning-Based Approaches for Prediction of Binary Star Parameters
2023 5th Novel Intelligent and Leading Emerging Sciences Conference (NILES)
Year: 2023 | Conference Paper |
Cited by: Papers (1)
The precise computation of binary star parameters is crucial for understanding their formation, evolution, and dynamics. However, large datasets of available astronomical measurements require substantial effort for computing using classic astronomical methods. Deep learning (DL) is a promising approach that can provide a proper solution for estimating the parameters and reducing the burden of the ...Show More
The effect of massive binaries on stellar populations and supernova progenitors
We compare our latest single and binary stellar model results from the Cambridge stars code to several sets of observations. We examine four stellar population ratios: the number of blue to red supergiants, the number of Wolf–Rayet stars to O supergiants, the number of red supergiants to Wolf–Rayet stars and the relative number of Wolf–Rayet subtypes, WC to WN stars. These four ratios provide a qu...Show More
The growth of massive stars via stellar collisions in ensemble star clusters
Recent simulations and observations suggest that star clusters form via the assembling of smaller subclusters. Because of their short relaxation time, subclusters experience core collapse much earlier than virialized solo clusters, which have similar properties of the merger remnant of the assembling clusters. As a consequence, it seems that the assembling clusters result in efficient multiple col...Show More
G11.92−0.61 MM1: a Keplerian disc around a massive young proto-O star
The formation process of massive stars is not well understood, and advancement in our understanding benefits from high-resolution observations and modelling of the gas and dust surrounding individual high-mass (proto)stars. Here, we report subarcsecond (≲1550 au) resolution observations of the young massive star G11.92−0.61 MM1 with the Submillimeter Array (SMA) and Very Large Array (VLA). Our 1.3...Show More
A new model for the origin of very metal poor stars and their chemical composition
The genesis and chemical patterns of the metal-poor stars in the galactic halo remain an open question. Current models do not seem to give a satisfactory explanation for the observed abundances of lithium in the galactic metal-poor stars and the existence of carbon-enhanced metal-poor (CEMP) and nitrogen-enhanced metal-poor (NEMP) stars. In order to deal with some of these theoretical issues, we s...Show More
Molecular line study of massive star-forming regions from the Red MSX Source survey
In this paper, we have selected a sample of massive star-forming regions from the Red MSX Source survey, in order to study star formation activities (mainly outflow and inflow signatures). We have focused on three molecular lines from the Millimeter Astronomy Legacy Team Survey at 90 GHz: HCO+(1–0), H13CO+(1–0) and SiO(2–1). According to previous observations, our sources can be divided into two g...Show More
A comparison of the rotational properties of T Tauri stars in Orion and Taurus
We analyse the distribution of projected equatorial velocities (v sin i) for a magnitude-limited sample of stars in Taurus, in order to assess whether this sample can contain a population of fast rotators (missed in previous photometric monitoring campaigns) similar to those recently discovered in Orion by Stassun et al. We find strong evidence, in line with the results of photometric monitoring c...Show More
Bulk viscosity of mixed nucleon–hyperon–quark matter in neutron stars
We calculate the coefficient of bulk viscosity by considering the non-leptonic weak interactions in the cores of hybrid stars with both hyperons and quarks. We first determine the dependence of the production rate of neutrons on the reaction rate of quarks in the non-leptonic processes, that is, $\Gamma_n=K_S\ \Gamma_S\ +\ \Gamma_\Lambda\ +\ 2\Gamma_{\Sigma-}$. The conversion rate, K s , in our sc...Show More
X-rays from massive OB stars: thermal emission from radiative shocks
Chandra grating spectra of a sample of 15 massive OB stars were analysed under the basic assumption that the X-ray emission is produced in an ensemble of shocks formed in the winds driven by these objects. Shocks develop either as a result of radiation-driven instabilities or due to confinement of the wind by a relatively strong magnetic field, and since they are radiative, a simple model of their...Show More
Testing stellar population models with star clusters in the Large Magellanic Cloud
We present high signal-to-noise ratio integrated spectra of 24 star clusters in the Large Magellanic Cloud (LMC), obtained using the FLAIR spectrograph at the UK Schmidt telescope. The spectra have been placed on to the Lick/IDS system in order to test the calibration of Simple Stellar Population (SSP) models.We have compared the SSP-predicted metallicities of the clusters with those from the lite...Show More
AGB stars in the SMC: evolution and dust properties based on Spitzer observations
We study the population of asymptotic giant branch (AGB) stars in the Small Magellanic Cloud (SMC) by means of full evolutionary models of stars of mass 1 M⊙ ≤ M ≤ 8 M⊙, evolved through the thermally pulsing phase. The models also account for dust production in the circumstellar envelope. We compare Spitzer infrared colours with results from theoretical modelling. We show that ∼75 per cent of the ...Show More
Nearly uniform internal rotation of solar-like main-sequence stars revealed by space-based asteroseismology and spectroscopic measurements
The rotation rates in the deep interior and at the surface of 22 main-sequence stars with masses between 1.0 and 1.6 M⊙ are constrained by combining asteroseismological analysis with spectroscopic measurements. The asteroseismic data of each star are taken by the Kepler or CoRoT space mission. It is found that the difference between the surface rotation rate and the average rotation rate (excludin...Show More
PARSEC evolutionary tracks of massive stars up to 350 M⊙ at metallicities 0.0001 ≤ Z ≤ 0.04
We complement the PARSEC data base of stellar evolutionary tracks with new models of massive stars, from the pre-main-sequence phase to the central carbon ignition. We consider a broad range of metallicities, 0.0001 ≤ Z ≤ 0.04 and initial masses up to Mini = 350 M⊙. The main difference with respect to our previous models of massive stars is the adoption of a recent formalizm accounting for the mas...Show More
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