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Journal articles on the topic 'Solar-type star'

Author: Grafiati

Published: 4 June 2021

Last updated: 19 February 2022

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1

Smith, Keith T. "Is the Sun a solar-type star?" Science 357, no. 6347 (2017): 159.1–159. http://dx.doi.org/10.1126/science.357.6347.159-a.

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2

Mirzoyan, L. V. "Flare stars in star clusters, associations and solar vicinity." Symposium - International Astronomical Union 137 (1990): 1–13. http://dx.doi.org/10.1017/s0074180900187303.

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The observational data on flare stars observed in star clusters and associations as well as in the solar vicinity (the UV Ceti type stars) are discussed. The analysis of these data show that they constitute one common class of objects possessing flare activity and the differences between them are conditioned by the age differences. The stage of flare activity is an evolutionary stage, one of the earliest stages of evolution passed by all red dwarf stars. It comes before the end of their T Tau stage of evolution. The UV Ceti type flare stars in the solar vicinity seem to be the population of th

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3

He, Han, Huaning Wang, Yan Yan, and Duo Yun. "Magnetic Activity Discrepancies of Solar-Type Stars Revealed by Kepler Light Curves." Proceedings of the International Astronomical Union 13, S335 (2017): 7–10. http://dx.doi.org/10.1017/s1743921317007670.

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AbstractMagnetic activity information is concealed in the shape of stellar light curves owing to the process of rotational modulation. We developed approaches to extract magnetic activity characteristics from stellar light curves, and applied the method to a solar-type star observed with Kepler space telescope and also to the Sun for comparison. The result reveals distinct magnetic activity discrepancies between the solar-type star and the Sun. (1) The light-curve periodicity of the solar-type star is generally stronger than that of the Sun. (2) For the solar-type star, when the range of light

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Roberts, Lewis C., Andrei Tokovinin, Brian D. Mason, William I. Hartkopf, and Reed L. Riddle. "OBSERVATIONS OF HIERARCHICAL SOLAR-TYPE MULTIPLE STAR SYSTEMS." Astronomical Journal 150, no. 4 (2015): 130. http://dx.doi.org/10.1088/0004-6256/150/4/130.

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5

Porto de Mello, G. F., and L. da Silva. "HR 6094: A Young Solar-Type, Solar-Metallicity Barium Dwarf Star." Astrophysical Journal 476, no. 2 (1997): L89—L92. http://dx.doi.org/10.1086/310504.

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da Silva, L., and G. F. Porto de Mello. "Lithium Abundances in Solar-Type Stars." Symposium - International Astronomical Union 198 (2000): 495–97. http://dx.doi.org/10.1017/s0074180900167142.

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We report Li abundances from the λ6707 line for 19 nearby dwarf and subgiant solar-type stars. The unevolved stars in this sample present high (> 2.00) Li abundances. We found a few cases of subgiant stars which present high Li content. The Sun seems to be part of a population of nearly unevolved stars which have depleted their Li to a high degree: all other metal-normal, near ZAMS stars in our sample show higher than solar Li content. There seems to be no correlation of the degree of Li depletion with mass, atmospheric parameters or state of evolution: as an example we found a star (HR1532

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7

Mayor, Michel, and Didier Queloz. "A Jupiter-mass companion to a solar-type star." Nature 378, no. 6555 (1995): 355–59. http://dx.doi.org/10.1038/378355a0.

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8

Soderblom, David R. "Determining the temperatures of solar-type stars - Do star spots produce color anomalies?" Astrophysical Journal 342 (July 1989): 823. http://dx.doi.org/10.1086/167639.

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9

Brown, Carolyn, Brad Carter, Stephen Marsden, and Ian Waite. "Starspots on Young Solar-Type Stars." Proceedings of the International Astronomical Union 9, S302 (2013): 148–49. http://dx.doi.org/10.1017/s1743921314001938.

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AbstractDoppler Imaging of starspots on young solar analogues is a way to investigate the early history of solar magnetic activity by proxy. Doppler images of young G-dwarfs have yielded the presence of large polar spots, extending to moderate latitudes, along with measurements of the surface differential rotation. The differential rotation measurement for one star (RX J0850.1-7554) suggests it is possibly the first example of a young G-type dwarf whose surface rotates as almost a solid body, in marked contrast to the differential rotation of other rapidly rotating young G-dwarfs and the prese

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10

Barker, Adrian J., and Gordon I. Ogilvie. "Internal wave breaking and the fate of planets around solar-type stars." Proceedings of the International Astronomical Union 6, S271 (2010): 363–64. http://dx.doi.org/10.1017/s1743921311017807.

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AbstractInternal gravity waves are excited at the interface of convection and radiation zones of a solar-type star, by the tidal forcing of a short-period planet. The fate of these waves as they approach the centre of the star depends on their amplitude. We discuss the results of numerical simulations of these waves approaching the centre of a star, and the resulting evolution of the spin of the central regions of the star and the orbit of the planet. If the waves break, we find efficient tidal dissipation, which is not present if the waves perfectly reflect from the centre. This highlights an

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11

Soderblom, David R. "Using lithium to estimate ages for solar-type stars." Proceedings of the International Astronomical Union 5, S268 (2009): 359–60. http://dx.doi.org/10.1017/s1743921310004461.

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12

Gough, D. O., and E. Novotny. "The Asteroseismic Calibration of Solar-Type Stars." International Astronomical Union Colloquium 137 (1993): 550–53. http://dx.doi.org/10.1017/s0252921100018418.

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AbstractThe addition of seismic parameters to stellar-model calibrations substantially increases the constraints one can place on the properties of stars. We present some preliminary calculations to assess the accuracy with which certain stellar parameters can be inferred. For simplicity we use just two of the three most basic seismic parameters characterizing the low-degree p modes that might be measured from intensity variations by instruments such as photometers planned for the ESA spacecraft PRISMA. We ascertain the accuracy of a calibration of an isolated star and of a cluster of N solar-

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13

Kamp, Inga, and Fatima Sammar. "Circumstellar Disks around Young Solar-type Stars." Symposium - International Astronomical Union 219 (2004): 385–89. http://dx.doi.org/10.1017/s0074180900182361.

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The chemistry of circumstellar disks around young (a few 10 Myr) solar-type stars is mainly driven by the strong UV radiation field of the central star. As a starting point for a detailed UV radiation field, the rocket and satellite observations of the solar chromosphere are used and scaled according to the time-dependent behaviour of stellar activity. The disk chemistry as well as dust and gas temperatures are then derived self-consistently from the model. The results of these calculations can be used for the identification of the most promising gas tracers as well as for the interpretation o

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14

Käpylä, P. J. "Star-in-a-box simulations of fully convective stars." Astronomy & Astrophysics 651 (July 2021): A66. http://dx.doi.org/10.1051/0004-6361/202040049.

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Context. Main-sequence late-type stars with masses of less than 0.35 M⊙ are fully convective. Aims. The goal is to study convection, differential rotation, and dynamos as functions of rotation in fully convective stars. Methods. Three-dimensional hydrodynamic and magnetohydrodynamic numerical simulations with a star-in-a-box model, in which a spherical star is immersed inside of a Cartesian cube, are used. The model corresponds to a 0.2 M⊙ main-sequence M5 dwarf. A range of rotation periods (Prot) between 4.3 and 430 d is explored. Results. The slowly rotating model with Prot = 430 days produc

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15

Jardine, M., J. Barnes, Y. Unruh, and A. Collier Cameron. "Prominences on Rapidly-Rotating Solar-Type Stars." International Astronomical Union Colloquium 167 (1998): 235–38. http://dx.doi.org/10.1017/s0252921100047655.

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AbstractWe present Hα observations of two rapidly-rotating G2 dwarfs in the Alpha Persei cluster and of AB Dor, a young K0 dwarf. All three stars have projected rotational velocities of about 90 km s−1 and axial rotation periods ranging from 11 to 15 hours. He 520 and AB Dor show very clear transient features that move through the profile. The most likely explanation for these features is that they are huge prominences in co-rotation with the star. We also use the recently developed technique of least squares deconvolution to present simultaneous dynamic profiles of the stars’ photospheric lin

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16

Giampapa, Mark S. "The Photometric Variability of Solar-Type Stars." Proceedings of the International Astronomical Union 11, A29A (2015): 365–71. http://dx.doi.org/10.1017/s174392131600329x.

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AbstractThe joint variability of chromospheric emission with the integrated flux in the Kepler visible band for the Sun as a star is examined. No correlation between our Ca II K line parameter and the Kepler passband is seen, suggesting that visible-band variability in solar-like stars is mostly independent of solar-like chromospheric activity. However, the K-line parameter time series and the total solar flux in the infrared K band appear weakly correlated, reflecting the wavelength dependence of the relationship between magnetic activity and broadband variability. We then apply a schematic,

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17

Zubrin, Robert. "Exchange of material between solar systems by random stellar encounters." International Journal of Astrobiology 19, no. 1 (2019): 43–48. http://dx.doi.org/10.1017/s1473550419000144.

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AbstractIt is shown that a mechanism involving only random motion of the sun with respect to the surrounding star field can account for the ~1 per 25 Myr characteristic frequency of large cometary impacts on Earth. In the proposed mechanism, the sun travels through the Oort Cloud of an encounter star, most typically a Type M dwarf, while the dwarf flies through the Oort cloud of our Sun. As a result, Oort Cloud objects from our Solar System are precipitated in large numbers to impact planets in the dwarf star system, while the dwarf's Oort Cloud objects are destabilized to impact planets in ou

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18

Queloz, Didier, and Mejd Alsari. "The Discovery of the First Exoplanet Orbiting a Solar-Type Star." Scientific Video Protocols 1, no. 1 (2020): 1–3. http://dx.doi.org/10.32386/scivpro.000017.

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Didier Queloz is Professor of Physics at the Cavendish Laboratory (University of Cambridge) and Geneva University. He was jointly awarded the 2019 Nobel Prize in Physics for “the discovery of an exoplanet orbiting a solar-type star”. In the first part of his conversation with Mejd Alsari he discusses the impact of his 1995 discovery on the theory of planetary systems formation.

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19

Short, C. I., and P. H. Hauschildt. "A Non‐LTE Line‐Blanketed Model of a Solar‐Type Star." Astrophysical Journal 618, no. 2 (2005): 926–38. http://dx.doi.org/10.1086/426128.

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20

Favata, F., G. Micela, S. Orlando, J. H. M. M. Schmitt, S. Sciortino, and J. Hall. "The X-ray cycle in the solar-type star HD 81809." Astronomy & Astrophysics 490, no. 3 (2008): 1121–26. http://dx.doi.org/10.1051/0004-6361:200809694.

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21

Théado, Sylvie, Elise Bohuon, and Sylvie Vauclair. "Lithium destruction induced by planetary accretion in solar-type stars." Proceedings of the International Astronomical Union 5, S268 (2009): 427–28. http://dx.doi.org/10.1017/s1743921310004588.

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AbstractAccretion of planetary (metal-rich) material onto a star in its early phases can produce episodes of thermohaline convection below the outer convective zone. These extra-mixing phases lead to rapid lithium destruction. The observed dispersion of lithium abundances in solar-type stars can be related to such events.

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22

Sheminova, V. A. "The line asymmetry in the spectra of the Sun and solar-type stars." Kinematika i fizika nebesnyh tel (Online) 36, no. 6 (2020): 65–87. http://dx.doi.org/10.15407/kfnt2020.06.065.

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We have analysed the asymmetry of lines Fe I and Fe II in spectra of a solar flux using three FTS atlases and the HARPS atlas and also in spectra of 13 stars using observation data on the HARPS spectrograph. To reduce observation noise individual line bisectors of each star have been averaged. The obtained average bisectors in the stellar spectra are more or less similar to the shape C well known to the Sun. In stars with rotation velocities greater than 5 km/s the shape of the bisectors is more like /. The curvature and span of the bisectors increase with the temperature of the star. Our resu

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23

Gallet, F., C. Zanni, and L. Amard. "Rotational evolution of solar-type protostars during the star-disk interaction phase." Astronomy & Astrophysics 632 (November 21, 2019): A6. http://dx.doi.org/10.1051/0004-6361/201935432.

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Context. The early pre-main sequence phase during which solar-mass stars are still likely surrounded by an accretion disk represents a puzzling stage of their rotational evolution. While solar-mass stars are accreting and contracting, they do not seem to spin up substantially. Aims. It is usually assumed that the magnetospheric star-disk interaction tends to maintain the stellar rotation period constant (“disk-locking”), but this hypothesis has never been thoroughly verified. Our aim is to investigate the impact of the star-disk interaction mechanism on the stellar spin evolution during the ac

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24

He, Han, Huaning Wang, Mei Zhang, Ahmad Mehrabi, Yan Yan, and Duo Yun. "Phase difference between long-term magnetic feature activity and flare activity of solar-type stars." Proceedings of the International Astronomical Union 13, S340 (2018): 217–20. http://dx.doi.org/10.1017/s1743921318000960.

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AbstractIn the light curves of some solar-type stars, both rotational modulation (caused by corotating bright or dark magnetic features) and flare phenomena can be seen simultaneously. Based on these light curve observations, the relation between stellar magnetic feature activity (reflected by the rotational modulation component of the light curves) and flare activity can be investigated. Here, we analyze the light curve data of a flare-abundant solar-type star, KIC 6034120, observed with Kepler space telescope, and describe magnetic feature activity property by fluctuation range of light curv

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25

Barnes, Sydney, Sabatino Sofia, and Marc Pinsonneault. "Disk Locking and the Presence of Slow Rotators among Solar‐Type Stars in Young Star Clusters." Astrophysical Journal 548, no. 2 (2001): 1071–80. http://dx.doi.org/10.1086/318988.

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26

Namekata, Kosuke, James R. A. Davenport, Brett M. Morris, et al. "Temporal Evolution of Spatially Resolved Individual Star Spots on a Planet-hosting Solar-type Star: Kepler-17." Astrophysical Journal 891, no. 2 (2020): 103. http://dx.doi.org/10.3847/1538-4357/ab7384.

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27

Matloff, Gregory L., and John Pazmino. "Detecting Interstellar Migrations." International Astronomical Union Colloquium 161 (January 1997): 757–59. http://dx.doi.org/10.1017/s0252921100015360.

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AbstractInterstellar Migrations may occur when a civilization’s star enters the Red Giant phase, thereby dooming the life-bearing planet(s). Ecologically self-contained «world ships», massing billions of kilograms and propelled by hyperthin, space-manufactured solar sails thousands of kilometers in diameter unfurled near the home star are possible vehicles to transfer a threatened civilization to a neighboring star. Consideration of the nearest Red Giants reveals that Pollux is the nearest formerly solar-type Red Giant. Known stellar neighbors of Pollux are surveyed to determine likely directi

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28

Roberts, Lewis C., Andrei Tokovinin, Brian D. Mason, and Anne D. Marinan. "Continued Kinematic and Photometric Investigations of Hierarchical Solar-type Multiple Star Systems." Astronomical Journal 153, no. 3 (2017): 100. http://dx.doi.org/10.3847/1538-3881/153/3/100.

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29

Ayal, Shai, Mario Livio, and Tsvi Piran. "Tidal Disruption of a Solar‐Type Star by a Supermassive Black Hole." Astrophysical Journal 545, no. 2 (2000): 772–80. http://dx.doi.org/10.1086/317835.

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30

Donahue, Robert A., and Sallie L. Baliunas. "Evidence of differential surface rotation in the solar-type star HD 114710." Astrophysical Journal 393 (July 1992): L63. http://dx.doi.org/10.1086/186452.

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31

Lefloch, Bertrand, C. Vastel, S. Viti, et al. "Phosphorus-bearing molecules in solar-type star-forming regions: first PO detection." Monthly Notices of the Royal Astronomical Society 462, no. 4 (2016): 3937–44. http://dx.doi.org/10.1093/mnras/stw1918.

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32

Lebreton, J., J. C. Augereau, W. F. Thi, et al. "An icy Kuiper belt around the young solar-type star HD 181327." Astronomy & Astrophysics 539 (February 20, 2012): A17. http://dx.doi.org/10.1051/0004-6361/201117714.

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von Rekowski, B., and N. Piskunov. "Global 3-D solar-type star-disc dynamo systems: I. MHD modeling." Astronomische Nachrichten 327, no. 4 (2006): 340–54. http://dx.doi.org/10.1002/asna.200510526.

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34

Buccino, Andrea P., Mariela C. Vieytes та Pablo J. D. Mauas. "A statistical analysis of Hα-Ca II relation for solar-type stars of different activity levels". Proceedings of the International Astronomical Union 7, S286 (2011): 324–27. http://dx.doi.org/10.1017/s1743921312005030.

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AbstractBased on our large spectral database obtained at CASLEO Argentinian Observatory, we analyzed the relation between simultaneous measurements of Hα and Ca ii H+K fluxes. Although the correlation between both proxies is positive for the solar case, in 2007 our group found that while some stars exhibit correlations between Hα and the Ca ii lines, the slopes change from star to star, including cases where no correlation was found. To discern if this flux-flux relation depends on the level of activity of the star and if it is associated with the distribution of active regions in the stellar

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35

Charbonneau, Paul, and Keith B. Macgregor. "Spin-Down of Solar-Type Stars with Internal Magnetic Fields." International Astronomical Union Colloquium 137 (1993): 464–68. http://dx.doi.org/10.1017/s0252921100018261.

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AbstractWe present a selection of results from a large set of numerical simulations of the spin-down of a solar-type star containing a large scale magnetic field in its radiative interior. Our computations are dynamical, in that they take into account both the generation of the toroidal component by the wind-induced shear endits back-reaction on the azimuthal flow. Our results demonstrate the existence of classes of internal magnetic fields that can accomodate rapid spin-down near the ZAMS, and yield weak internal differential rotation by the solar age.

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36

Nissen, P. E., J. Christensen-Dalsgaard, J. R. Mosumgaard, V. Silva Aguirre, E. Spitoni, and K. Verma. "High-precision abundances of elements in solar-type stars." Astronomy & Astrophysics 640 (August 2020): A81. http://dx.doi.org/10.1051/0004-6361/202038300.

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Aims. Previous high-precision studies of abundances of elements in solar twin stars are extended to a wider metallicity range to see how the trends of element ratios with stellar age depend on [Fe/H]. Methods. HARPS spectra with signal-to-noise ratios S/N ≳ 600 at λ ∼ 6000 Å were analysed with MARCS model atmospheres to obtain 1D LTE abundances of C, O, Na, Mg, Al, Si, Ca, Ti, Cr, Fe, Ni, Sr, and Y for 72 nearby solar-type stars with metallicities in the range of −0.3 ≲ [Fe/H] ≲ +0.3 and ASTEC stellar models were used to determine stellar ages from effective temperatures, luminosities obtain

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Flores, M., J. F. González, M. Jaque Arancibia, et al. "HD 38858: a solar-type star with an activity cycle of ∼10.8 yr." Astronomy & Astrophysics 620 (November 27, 2018): A34. http://dx.doi.org/10.1051/0004-6361/201833330.

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Context. The detection of chromospheric activity cycles in solar-analogue and twin stars can be used to place the solar cycle in a wider context. However, relatively few of these stars with activity cycles have been detected. It is well known that the cores of the Ca II H&K lines are modulated by stellar activity. The behaviour of the Balmer and other optical lines with stellar activity is not yet completely understood. Aims. We search for variations in the Ca II H&K, Balmer, and Fe II lines modulated by stellar activity. In particular, we apply a novel strategy to detect possible shap

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Bladh, S., K. Eriksson, P. Marigo, S. Liljegren, and B. Aringer. "Carbon star wind models at solar and sub-solar metallicities: a comparative study." Astronomy & Astrophysics 623 (March 2019): A119. http://dx.doi.org/10.1051/0004-6361/201834778.

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Context. The heavy mass loss observed in evolved stars on the asymptotic giant branch (AGB) is usually attributed to dust-driven winds, but it is still an open question how much AGB stars contribute to the dust production in the interstellar medium, especially at lower metallicities. In the case of C-type AGB stars, where the wind is thought to be driven by radiation pressure on amorphous carbon grains, there should be significant dust production even in metal-poor environments. Carbon stars can manufacture the building blocks needed to form the wind-driving dust species themselves, irrespecti

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Mittag, M., J. H. M. M. Schmitt, T. S. Metcalfe, A. Hempelmann, and K. P. Schröder. "Magnetic activity of the solar-like star HD 140538." Astronomy & Astrophysics 628 (August 2019): A107. http://dx.doi.org/10.1051/0004-6361/201935654.

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The periods of rotation and activity cycles are among the most important properties of the magnetic dynamo thought to be operating in late-type, main-sequence stars. In this paper, we present a SMWO-index time series composed from different data sources for the solar-like star HD 140538 and derive a period of 3.88 ± 0.02 yr for its activity cycle. Furthermore, we analyse the high-cadence, seasonal SMWO data taken with the TIGRE telescope and find a rotational period of 20.71 ± 0.32 days. In addition, we estimate the stellar age of HD 140538 as 3.7 Gyrs via a matching evolutionary track. This i

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Raghavan, Deepak, H. A. McAlister, T. J. Henry, and B. D. Mason. "A Survey of Stellar Families: Multiplicity Among Solar-type Stars." Proceedings of the International Astronomical Union 2, S240 (2006): 254–57. http://dx.doi.org/10.1017/s1743921307004115.

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AbstractStellar multiplicity is a fundamental astrophysical property. In addition to being the only physical basis for accurate mass determination, this parameter is believed to influence important aspects such as planet formation and stability. Contrary to earlier expectations, recent studies have shown that even against selection biases, as many as 23% of the planetary systems reside in multiple star systems (Raghavan et al. 2006)). Leveraging recent efforts in identifying stellar and substellar companions to solar-type stars, and augmenting them with targeted observations, we are conducting

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Kallinger, T. "MOST found evidence for solar-type oscillations in the K2 giant star HD20884." Communications in Asteroseismology 153 (2008): 84–102. http://dx.doi.org/10.1553/cia_153s84.

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Brown, Benjamin P., Mark S. Miesch, Matthew K. Browning, Allan Sacha Brun, and Juri Toomre. "MAGNETIC CYCLES IN A CONVECTIVE DYNAMO SIMULATION OF A YOUNG SOLAR-TYPE STAR." Astrophysical Journal 731, no. 1 (2011): 69. http://dx.doi.org/10.1088/0004-637x/731/1/69.

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43

Kovács, G., G. Á. Bakos, J. D. Hartman, et al. "HAT-P-15b: A 10.9 DAY EXTRASOLAR PLANET TRANSITING A SOLAR-TYPE STAR." Astrophysical Journal 724, no. 2 (2010): 866–77. http://dx.doi.org/10.1088/0004-637x/724/2/866.

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44

Gillon, M., A. P. Doyle, M. Lendl, et al. "WASP-50 b: a hot Jupiter transiting a moderately active solar-type star." Astronomy & Astrophysics 533 (September 2011): A88. http://dx.doi.org/10.1051/0004-6361/201117198.

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Buccino, A. P., L. Sraibman, P. M. Olivar та F. O. Minotti. "An application of a solar-type dynamo model for ε Eridani". Monthly Notices of the Royal Astronomical Society 497, № 3 (2020): 3968–75. http://dx.doi.org/10.1093/mnras/staa1908.

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ABSTRACT During the last decade, the relation between activity cycle periods and stellar parameters has received special attention. The construction of reliable registries of activity reveals that solar-type stars exhibit activity cycles with periods from few years to decades and, in some cases, long and short activity cycles coexist suggesting that two dynamos could operate in these stars. In particular, ε Eridani is an active young K2V star (0.8 Gyr), which exhibits short and long-term chromospheric cycles of ∼3 and ∼13-yr periods. Additionally, between 1985 and 1992, the star went through a

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Jiang, S. Y. "The history of KZ Hya and its unseen companions." Proceedings of the International Astronomical Union 4, S252 (2008): 421–22. http://dx.doi.org/10.1017/s1743921308023375.

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AbstractKZ Hya is a short-period high amplitude metal pool population II pulsating variable. Its spectral type is B9-A7 III/IV. Its average effective temperature is 7640K. But its mass is only 0.97 solar mass. From normal stellar evolution and H-R diagram, we can not get such a solar mass star at post main sequence stage with so high effective temperature and so early type spectra. We observe this star since 1984 till now, 23years past. Finally we prove it is inside a binary with at least 2 unseen companions. The most massive companion has mass larger than 0.76 solar mass, mostly may be 0.99 t

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Rao, Suvrat, Camilla Pezzotti, Georges Meynet, et al. "Star-planet interactions." Astronomy & Astrophysics 651 (July 2021): A50. http://dx.doi.org/10.1051/0004-6361/202039965.

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Context. Tidal interactions and planetary evaporation processes impact the evolution of close-in star–planet systems. Aims. We study the impact of stellar rotation on these processes. Methods. We compute the time evolution of star–planet systems consisting of a planet with an initial mass between 0.02 and 2.5 MJup (6 and 800 MEarth) in a quasi-circular orbit with an initial orbital distance between 0.01 and 0.10 au, around a solar-type star evolving from the pre-main-sequence (PMS) phase until the end of the main-sequence phase. We account for the evolution of: the stellar structure, the stell

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Bertulani, C. A., M. Naizer, and W. Newton. "Stellar oscillations induced by the passage of a fast stellar object." International Journal of Modern Physics D 23, no. 10 (2014): 1450084. http://dx.doi.org/10.1142/s0218271814500849.

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In this paper, we investigate induced oscillations by the gravitational field of a fast stellar object, such as a neutron star or a black-hole in a near miss collision with another star. Nonadiabatic collision conditions may lead to large amplitude oscillations in the star. We show that for a solar-type star a resonant condition can be achieved by a fast moving stellar object with velocity in the range of 100 to 1000 km/s, passing at a distance of a few multiples of the star radius. Although such collisions are rare, they are more frequent than head-on collisions, and their effects could be ob

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Eberle, J., M. Cuntz, B. Quarles, and Z. E. Musielak. "Case studies of habitable Trojan planets in the system of HD 23079." International Journal of Astrobiology 10, no. 4 (2011): 325–34. http://dx.doi.org/10.1017/s1473550411000176.

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AbstractWe investigate the possibility of habitable Trojan planets in the HD 23079 star–planet system. This system consists of a solar-type star and a Jupiter-type planet, which orbits the star near the outer edge of the stellar habitable zone in an orbit of low eccentricity. We find that in agreement with previous studies Earth-mass habitable Trojan planets are possible in this system, although the success of staying within the zone of habitability is significantly affected by the orbital parameters of the giant planet and by the initial condition of the theoretical Earth-mass planet. In one

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Marsden, Stephen, Pascal Petit, Sandra Jeffers, Jose-Dias do Nascimento, Bradley Carter, and Carolyn Brown. "A Bcool spectropolarimetric survey of over 150 solar-type stars." Proceedings of the International Astronomical Union 9, S302 (2013): 138–41. http://dx.doi.org/10.1017/s1743921314001896.

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AbstractAs part of the Bcool project, over 150 solar-type stars chosen mainly from planet search databases have been observed between 2006 and 2013 using the NARVAL and ESPaDOnS spectropolarimeters on the Telescope Bernard Lyot (Pic du Midi, France) and the Canada France Hawaii Telescope (Mauna Kea, USA), respectively. These single “snapshot” observations have been used to detect the presence of magnetic fields on 40% of our sample, with the highest detection rates occurring for the youngest stars. From our observations we have determined the mean surface longitudinal field (or an upper limit

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