Rotation in the Pleiades With K2: III. Speculations on origins and evolution by Stauffer, J, Rebull, L, Bouvier, J, Hillenbrand, L, Collier-Cameron, A, Pinsonneault, M, Aigrain, S, Barrado, D, Bouy, H, Ciardi, D, Cody, A, David, T, Micela, G, Soderblom, D, Somers, G, Stassun, K, Valenti, J, Vrba, F

“…During pre-main-sequence evolution from ∼3 Myr (NGC 2264 age) to ∼125 Myr (Pleiades age), stars of 0.3 shed about half of their angular momentum, with the fractional change in period between 3 and 125 Myr being nearly independent of mass for fully convective stars. …”

Brown dwarfs in retrogradely precessing cataclysmic variables? by Martin E.L., Deshpande R., Montgomery M.M.

“…We compare Smoothed Particle Hydrodynamic simulations of retrogradely precessing accretion disks that have a white dwarf primary and a main sequence secondary with observational data and with theory on retrograde precession via tidal torques like those by the Moon and the Sun on the Earth [1, 2]. …”
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COGNITIVE APPROACH TO THE STUDY OF MINING TERMS – ENGLISH VERBS WITH A POSTPOSITION by R. V. Mershiev

“…To reach this goal of the study the main sequence of stages of the process of mining production was found out. …”
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Origin of the rotation rates of single white dwarfs and neutron stars by Spruit, H

“…The cores of giants are then very slowly rotating, and the rotation of white dwarfs and neutron stars is not a remnant of the rotation of their main sequence progenitors. The kicks associated with the observed proper motions of pulsars can explain the rotation rates of neutron stars, while slight non-axisymmetries in the mass loss during planetary nebula formation can explain the observed rotation of white dwarfs.…”

Massive star mergers: Induced mixing and nucleosynthesis by Ivanova, N, Podsiadlowski, P

“…The systems of interest are close binaries, initially consisting of a massive red supergiant and a main-sequence companion of a few solar masses. We apply parameterized results based on hydrodynamical simulations to model the stream-core interaction and the response of the star in a standard stellar-evolution code. …”

Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5 by J. Takata, A. K. H. Kong, X. F. Wang, F. F. Song, J. Mao, X. Hou, C.-P. Hu, L. C.-C. Lin, K. L. Li, C. Y. Hui

“…The stellar oscillation of the M-type main-sequence star has been predicted in theoretical studies, but no observational confirmation has been done. …”
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Can Self-Replicating Species Flourish in the Interior of a Star? by Luis A. Anchordoqui, Eugene M. Chudnovsky

“…Going against this dogma, we argue that an advanced form of life based upon short-lived species can exist inside main-sequence stars like our Sun.…”
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Proton-Induced Reactions of Astrophysical Interest by Chillery Thomas

“…A discrepancy exists between the 6Li abundances predicted from big bang nucleosynthesis models and those measured in pre-main sequence stars. To further constrain the predicted abundances of 6Li in these stars, high accuracy measurements are required of reactions destroying 6Li. …”
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Follow-Up of Extended Shells around B[e] Stars by Tiina Liimets, Michaela Kraus, Alexei Moiseev, Nicolas Duronea, Lydia Sonia Cidale, Cecilia Fariña

“…B[e] stars are massive B type emission line stars in different evolutionary stages ranging from pre-main sequence to post-main sequence. Due to their mass loss and ejection events these objects deposit huge amounts of mass and energy into their environment and enrich it with chemically processed material, contributing significantly to the chemical and dynamical evolution of their host galaxies. …”
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The X-Ray Emission Reveals the Coronal Activities of Semi-detached Binaries by Junhui Liu, Jianfeng Wu

“…We found that EBXs with main-sequence components exhibit an upward and then a downward trend in both the $\mathrm{log}{T}_{\mathrm{eff}}$ – $\mathrm{log}{L}_{{\rm{X}}}$ and M – $\mathrm{log}{L}_{{\rm{X}}}$ relations, which is different from the monotonically decreasing trend shown by EBXs containing sub-giant and giant components. …”
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The Age Distribution of Stellar Orbit Space Clumps by Verena Fürnkranz, Hans-Walter Rix, Johanna Coronado, Rhys Seeburger

“…It then entails isochrone fitting that accounts for: (a) widely varying distances and reddenings; (b) outliers and binaries; (c) sparsely populated main-sequence turnoffs, by incorporating the age information of the low-mass main sequence; and (d) the possible presence of an intrinsic age spread in the stellar population. …”
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Stellar Collisions in the Galactic Center: Massive Stars, Collision Remnants, and Missing Red Giants by Sanaea C. Rose, Smadar Naoz, Re’em Sari, Itai Linial

“…In this dense star cluster, direct collisions can occur between stars before they evolve off the main sequence. Using a statistical approach, we characterize the outcomes of these stellar collisions within the inner parsec of the Galactic center (GC). …”
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The Gas Accretion Rate of Star-forming Galaxies over the Last 4 Gyr by Apurba Bera, Nissim Kanekar, Jayaram N. Chengalur, Jasjeet S. Bagla

“…The average gas accretion rate onto the disk over the past 4 Gyr is similar to the average SFR over this period, implying that main-sequence galaxies have maintained a stable H i reservoir, despite the consumption of gas in star formation. …”
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Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 by Zhi Li, Yan Li

“…The rotating models start with a rotation rate of v _ini / v _crit = 0.4 at the zero-age main sequence, and the evolution is computed until the end of the central carbon-burning phase. …”
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The dust-continuum size of TNG50 galaxies at z = 1–5: a comparison with the distribution of stellar light, stars, dust, and H2 by Popping, Gergö, Pillepich, Annalisa, Calistro Rivera, Gabriela, Schulz, Sebastian, Hernquist, Lars, Kaasinen, Melanie, Marinacci, Federico, Nelson, Dylan, Vogelsberger, Mark

“…ABSTRACT We present predictions for the extent of the dust-continuum emission of main-sequence galaxies drawn from the TNG50 simulation in the range z = 1–5. …”
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High-Resolution Spectroscopy of Extremely Metal-Poor Stars from SDSS/SEGUE: I. Atmospheric Parameters and Chemical Compositions by Aoki, Wako, Beers, Timothy C., Lee, Young Sun, Honda, Satoshi, Ito, Hiroko, Takada-Hidai, Masahide, Frebel, Anna L., Suda, Takuma, Fujimoto, Masayuki Y., Carollo, Daniela, Sivarani, Thirupathi

“…Most of the sample (approximately 80%) are main-sequence turnoff stars, including dwarfs and subgiants. …”
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Near infrared spectroscopy and star-formation histories of 3 ≤ z ≤ 4 quiescent galaxies by Schreiber, C, Glazebrook, K, Nanayakkara, T, Kacprzak, G, Labbé, I, Oesch, P, Yuan, T, Tran, K, Papovich, C, Spitler, L, Straatman, C

“…We find specific star-formation rates (sSFR) lower than 0.15 Gyr−1 (a factor of ten below the main sequence) for all but one galaxy, and lower than 0.01 Gyr−1 for half of the sample. …”

GOODS-HERSCHEL AND CANDELS: THE MORPHOLOGIES OF ULTRALUMINOUS INFRARED GALAXIES AT z similar to 2 by Kartaltepe, J, Dickinson, M, Alexander, D, Bell, E, Dahlen, T, Elbaz, D, Faber, S, Lotz, J, McIntosh, D, Wiklind, T, Altieri, B, Aussel, H, Bethermin, M, Bournaud, F, Charmandaris, V, Conselice, C, Cooray, A, Dannerbauer, H, Dave, R, Dunlop, J, Dekel, A, Ferguson, H, Grogin, N, Hwang, H, Ivison, R

“…We investigate the position of the z ∼ 2 ULIRGs, along with 70 z ∼ 2 LIRGs, on the specific star formation rate versus redshift plane, and find 52 systems to be starbursts (i.e., they lie more than a factor of three above the main-sequence relation). We find that many of these systems are clear interactions and mergers (∼50%) compared to only 24% of systems on the main sequence relation. …”

Spectral fingerprints of earth-like planets around FGK stars by Rugheimer, S, Kaltenegger, L, Zsom, A, Segura, A, Sasselov, D

“… <p style="text-align:justify;"> We present model atmospheres for an Earth-like planet orbiting the entire grid of main sequence FGK stars with effective temperatures ranging from T_eff=4250 K to T_eff=7000 K in 250 K intervals. …”

The Early History of Stellar Spin: the Theory of Accretion onto Young Stellar Objects by Pudritz Ralph E., Matt Sean

“…The resolution of this issue is crucial for understanding the origin of the spins of pre main sequence stars. A significant fraction of these rotate very slowly, which indicates that an efficient angular momentum transport mechanism is at work to counteract the strong accretion spin up torques. …”
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