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Journal articles on the topic 'Stars: individual (Fomalhaut A)'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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1

Ruban, E. V., and A. A. Arkharov. "Young stars in gas-dust disks. I. Fomalhaut." Astrophysics 55, no. 1 (2012): 53–69. http://dx.doi.org/10.1007/s10511-012-9222-0.

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Stamm, Johann, Andrzej Czechowski, Ingrid Mann, Carsten Baumann, and Margaretha Myrvang. "Dust trajectory simulations around the Sun, Vega, and Fomalhaut." Astronomy & Astrophysics 626 (June 2019): A107. http://dx.doi.org/10.1051/0004-6361/201834727.

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Context. Vega and Fomalhaut display a thermal emission brightness that could possibly arise from hot dust near the stars, an inner extension of their planetary debris disks. An idea has been suggested that nanometer-sized dust particles are kept in the vicinity of the stars by electromagnetic forces. This resembles the trapping that model calculations show in the corotating magnetic field in the inner heliosphere within approximately 0.2 AU from the Sun. Aims. The aim of this work is to study whether the trapping of dust due to electromagnetic forces acting on charged dust near the Sun can occ

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3

Nielsen, Eric L., Michael C. Liu, Zahed Wahhaj, Beth A. Biller, and Thomas L. Hayward. "The Gemini NICI Planet-Finding Campaign: The Frequency of Giant Planets around Young B and A Stars." Proceedings of the International Astronomical Union 8, S299 (2013): 60–61. http://dx.doi.org/10.1017/s1743921313007874.

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AbstractWe have carried out high contrast imaging of 70 young, nearby B and A stars to search for brown dwarf and planetary companions as part of the Gemini NICI Planet-Finding Campaign. Our survey represents the largest, deepest survey for planets around high-mass stars (≈1.5–2.5 M⊙) conducted to date and includes the planet hosts β Pic and Fomalhaut. Despite detecting two new brown dwarfs, our observations did not detect new planets around our target stars, and we present upper limits on the fraction of high-mass stars that can host giant planets that are consistent with our null result.

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Di Folco, Emmanuel, Pierre Kervella, Frédéric Thévenin, Pierre Morel, Armando Domiciano de Suza та Vincent Coudé du Foresto. "Near-IR Observations of Vega-like Stars with the VLTI: β Pic, α PsA, ∊ Eri and τ Cet". Symposium - International Astronomical Union 219 (2004): 75–79. http://dx.doi.org/10.1017/s0074180900181975.

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We have conducted K band interferometric observations of four nearby main-sequence Vega-like stars at the VLTI with very long baselines. The very high resolution allowed us to probe the innermost region of the disks, where planets are supposed to be formed. The diameters of three bright and nearby prototypes β Pictoris, Fomalhaut (α PsA) and ∊ Eridani as well as τ Ceti have been measured with VINCI, the VLTI commissioning instrument, with a high accuracy. The derived diameters were used to constrain their age with help of the evolution code CESAM. The precision achieved with VINCI allowed us t

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5

Shannon, Andrew, Cathie Clarke, and Mark Wyatt. "Dancing with the stars: formation of the Fomalhaut triple system and its effect on the debris discs." Monthly Notices of the Royal Astronomical Society 442, no. 1 (2014): 142–47. http://dx.doi.org/10.1093/mnras/stu846.

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6

Su, Kate Y. L., and G. H. Rieke. "Signposts of Multiple Planets in Debris Disks." Proceedings of the International Astronomical Union 8, S299 (2013): 318–21. http://dx.doi.org/10.1017/s1743921313008764.

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AbstractWe review the nearby debris disk structures revealed by multi-wavelength images from Spitzer and Herschel, and complemented with detailed spectral energy distribution modeling. Similar to the definition of habitable zones around stars, debris disk structures should be identified and characterized in terms of dust temperatures rather than physical distances so that the heating power of different spectral type of stars is taken into account and common features in disks can be discussed and compared directly. Common features, such as warm (~150 K) dust belts near the water-ice line and co

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Padgett, Deborah L. "SpS1-Preparing for the harvest from large infrared surveys." Proceedings of the International Astronomical Union 5, H15 (2009): 510–11. http://dx.doi.org/10.1017/s1743921310010422.

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During the past decade, there has been a revolution in the availability of multi-wavelength astronomical surveys. From the Sloan Digital Sky Survey (SDSS) to the NRAO VLA Sky Survey (NVSS), astronomical research based on publicly accessible datasets is becoming standard practice in the community. Beginning with the Infrared Astronomical Satellite (IRAS) mission, infrared surveys have played a critical role in stellar astronomy by identifying cool and dusty stars worthy of spectroscopic characterization. IRAS' four photometric bands at 12, 25, 60, and 100 μm were ideal for detecting dusty circu

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Rebollido, I., C. Eiroa, B. Montesinos, et al. "The co-existence of hot and cold gas in debris discs." Astronomy & Astrophysics 614 (June 2018): A3. http://dx.doi.org/10.1051/0004-6361/201732329.

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Context. Debris discs have often been described as gas-poor discs as the gas-to-dust ratio is expected to be considerably lower than in primordial, protoplanetary discs. However, recent observations have confirmed the presence of a non-negligible amount of cold gas in the circumstellar (CS) debris discs around young main-sequence stars. This cold gas has been suggested to be related to the outgassing of planetesimals and cometary-like objects. Aims. The goal of this paper is to investigate the presence of hot gas in the immediate surroundings of the cold-gas-bearing debris-disc central stars.

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9

Heap, Sara R., Dennis Ebbets, Eliot M. Malumuth, Stephen P. Maran, Alex de Koter, and Ivan Hubeny. "GHRS Spectroscopy of individual stars in R136a." Astrophysical Journal 435 (November 1994): L39. http://dx.doi.org/10.1086/187589.

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10

Kennedy, Grant M. "The unexpected narrowness of eccentric debris rings: a sign of eccentricity during the protoplanetary disc phase." Royal Society Open Science 7, no. 6 (2020): 200063. http://dx.doi.org/10.1098/rsos.200063.

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This paper shows that the eccentric debris rings seen around the stars Fomalhaut and HD 202628 are narrower than expected in the standard eccentric planet perturbation scenario (sometimes referred to as ‘pericentre glow’). The standard scenario posits an initially circular and narrow belt of planetesimals at semi-major axis a , whose eccentricity is increased to e f after the gas disc has dispersed by secular perturbations from an eccentric planet, resulting in a belt of width 2 ae f . In a minor modification of this scenario, narrower belts can arise if the planetesimals are initially eccentr

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11

Baker, N., B. Szeidl, M. Breger, et al. "27. Variable Stars." Transactions of the International Astronomical Union 19, no. 1 (1985): 277–311. http://dx.doi.org/10.1017/s0251107x00006398.

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The field of variable-star research is so broad that no report of this nature could possibly mention all the papers that have appeared in the last three years. It is hoped, however, that the reviews below include the most important work and identify the most significant trends. This report comprises ten sections on as many different research topics, each written by a different member of Commission 27. In addition there are (in Section 12) three short reports about ongoing activities of the commission. The commission president is very grateful to the authors of the individual contributions who

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12

Hunter, Deidre A. "IC 10: a starburst galaxy resolved into individual stars." Symposium - International Astronomical Union 193 (1999): 484. http://dx.doi.org/10.1017/s0074180900206098.

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We present a preliminary analysis of HST images of the Local Group galaxy IC 10. IC 10 has an unusual Wolf-Rayet star population and is believed to be undergoing a starburst. Nevertheless, stars to at least 6.5 M⊙ are seen and the young star clusters are comparable in richness and spatial concentration to LMC populous clusters.

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13

Heggie, Douglas C., and Mirek Giersz. "Modelling Individual Globular Clusters." Proceedings of the International Astronomical Union 3, S246 (2007): 121–30. http://dx.doi.org/10.1017/s1743921308015469.

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AbstractAstronomers have constructed models of globular clusters for over 100 years. These models mainly fall into two categories: (i) static models, such as King's model and its variants, and (ii) evolutionary models. Most attention has been given to static models, which are used to estimate mass-to-light ratios and mass segregation, and to combine data from proper motions and radial velocities. Evolutionary models have been developed for a few objects using the gaseous model, the Fokker-Planck model, Monte Carlo models and N-body models. These models have had a significant role in the search

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Castanheira, B. G., and S. O. Kepler. "Seismological studies of ZZ Ceti stars - I. The model grid and the application to individual stars." Monthly Notices of the Royal Astronomical Society 385, no. 1 (2008): 430–44. http://dx.doi.org/10.1111/j.1365-2966.2008.12851.x.

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15

Whalen, Daniel J. "THE FIRST STARS." Acta Polytechnica 53, A (2013): 573–78. http://dx.doi.org/10.14311/ap.2013.53.0573.

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Pop III stars are the key to the character of primeval galaxies, the first heavy elements, the onset of cosmological reionization, and the seeds of supermassive black holes. Unfortunately, in spite of their increasing sophistication, numerical models of Pop III star formation cannot yet predict the masses of the first stars. Because they also lie at the edge of the observable universe, individual Pop III stars will remain beyond the reach of observatories for decades to come, and so their properties are unknown. However, it will soon be possible to constrain their masses by direct detection of

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16

Figueras, F., J. Torra, C. Jordi, and R. Asiain. "Age Determination for Am Stars." International Astronomical Union Colloquium 138 (1993): 634–38. http://dx.doi.org/10.1017/s0252921100021126.

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AbstractFrom uvby and Hβ photometry, individual stellar ages for A type stars have been derived using three different evolutionary models. In this paper we evaluate the corrections for metallicity and rotation to be applied to the physical parameters of Am and their influence on the determined ages. A test based on the Hyades open cluster is also presented.

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17

Guzik, J. A. "Delta Scuti Stars: Theory." Symposium - International Astronomical Union 185 (1998): 331–38. http://dx.doi.org/10.1017/s0074180900238904.

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The purpose of asteroseismology is not only to derive the internal structure of individual stars from their observed oscillation frequencies, but also to test and extend our understanding of the physics of matter under the extremes of temperature, density, and pressure found in stellar interiors. In this review, I hope to point out what we can learn about the Sun by studying δ Scuti stars, as well as what we can learn about stars more massive or evolved than the Sun. I will discuss some of the difficulties in theoretical approaches to asteroseismology for δ Scuti stars, using FG Vir, δ Scuti,

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18

Arentsen, Anke, Else Starkenburg, Matthew D. Shetrone, Alan W. McConnachie, Éric Depagne, and Kim A. Venn. "Binarity in CEMP-no stars." Proceedings of the International Astronomical Union 13, S334 (2017): 273–74. http://dx.doi.org/10.1017/s1743921317008171.

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AbstractWe monitor a sample of CEMP-no stars using the CFHT and SALT telescopes to gain additional knowledge about the possible binarity of these stars. This information is valuable for each individual star, and additionally it could be used to further constrain their binary fraction. We find two new CEMP-no binaries and four additional CEMP-no stars that show some indication of radial velocity variations, resulting in a CEMP-no binary fraction of ~20%.

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19

Quintana, Elisa V., Fred C. Adams, Jack J. Lissauer, and John E. Chambers. "Terrestrial Planet Formation around Individual Stars within Binary Star Systems." Astrophysical Journal 660, no. 1 (2007): 807–22. http://dx.doi.org/10.1086/512542.

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20

Taylor, A. R. "Radio Imaging of Symbiotic Stars." International Astronomical Union Colloquium 103 (1988): 77–83. http://dx.doi.org/10.1017/s0252921100103185.

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AbstractA brief review of radio observations of individual symbiotic stars is presented, with emphasis on radio imaging of the circumstellar nebulae. The ionized nebulae are catagorized into two types: outburst ejecta and stellar winds. Among the ejecta-type there is a strong tendency for bipolar or jet morphology. In the case of the quiescent, stellar wind emitter, a few very wide binary systems (eg. Hl-36) offer the potential of directly viewing the effects of the binary interaction.

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21

Breger, M., та N. Audard. "Observational asteroseismology of δ Scuti stars". Symposium - International Astronomical Union 181 (1997): 381–86. http://dx.doi.org/10.1017/s0074180900061295.

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Ground-based observational networks are now able to reliably detect more than 20 frequencies for individual δ Scuti stars. The ground-based Delta Scuti Network specializes in the intensive study of individual stars for several months with dedicated telescopes on different continents. With the new quantity and quality of data, the observational limit to extracting 50 or more frequencies in a single δ Scuti star is no longer determined only by the signal/noise ratio, but by the available frequency resolution.Recent results on the δ Scuti stars FG Vir and 4CVn are presented. 4CVn exhibits some of

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22

Gazzano, Jean-Christophe, Magali Deleuil, Patrick De Laverny, et al. "From stars to planets." Proceedings of the International Astronomical Union 4, S253 (2008): 404–5. http://dx.doi.org/10.1017/s174392130802677x.

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AbstractA large program of multi-fibre (FLAMES) spectroscopic observations of the stellar population in two CoRoT/Exoplanet field with the GIRAFFE/VLT, took place in spring 2008. It aims at characterizing the brightest dwarf population and providing the ground for statistical analysis of the planetary population found by CoRoT.To perform such an ambitious analysis, we use an automated software based on the MATISSE algorithm, originally designed for the GAIA/RVS spectral analysis. This software derives the atmospheric stellar parameters: effective temperature, surface gravity and the overall me

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23

Barbuy, B., S. Ortolani, M. Zoccali, et al. "Metal-poor globular clusters of the galactic bulge." Proceedings of the International Astronomical Union 5, S265 (2009): 344–45. http://dx.doi.org/10.1017/s1743921310000840.

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AbstractVery few abundance analyses of individual stars in metal-poor globular clusters in the galactic bulge are available. The main purpose of this study is to derive abundances in individual stars of such clusters, in order to establish their abundance pattern, trying to characterize the oldest bulge stellar populations.

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Herrero, Artemio. "Parameters of massive OB stars." Symposium - International Astronomical Union 212 (2003): 3–12. http://dx.doi.org/10.1017/s0074180900211583.

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I review our knowledge about effective temperatures and masses of massive OB stars paying special attention to results recently obtained using new atmospheric models including sphericity, mass-loss and line-blanketing. The new temperature scales for O dwarfs and supergiants are lower than previously accepted. No systematic mass discrepancy is found among O supergiants, although individual problematic cases still remain. It is shown that model atmospheres give answers consistent with binary systems. Good agreement is found between theoretical predictions and observations of the Wind Momentum-Lu

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Olevic, D., G. Popovic, and P. Jovanovic. "Recalculated orbits of 8 double stars." Serbian Astronomical Journal, no. 162 (2000): 109–13. http://dx.doi.org/10.2298/saj0062109o.

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The authors present new orbital elements for the following pairs: ADS 1227 ADS 3317, ADS 8128, ADS 8239, ADS 8242, ADS 8539, ADS 8949 and McA 61. Individual masses for these pairs are also calculated. For the pairs ADS 8128, ADS 8239, ADS 8539 and ADS 8949 calculated parallaxes are in accordance with the corresponding parallaxes of the Hipparchos Program.

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Clemens, J. Christopher. "Seismology of the ZZ Ceti Stars." Symposium - International Astronomical Union 185 (1998): 253–60. http://dx.doi.org/10.1017/s0074180900238734.

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The pulsations of white dwarf stars are potentially a rich source of information about white dwarf structural properties. Extracting and applying this information to improve our knowledge of white dwarf interiors requires measuring individual eigenperiods in a complex power spectrum, and identifying the character of the eigenmodes they represent. This review will summarize observational progress in these areas for the ZZ Ceti pulsators.

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Newberg, Heidi Jo. "Determining distances to stars statistically from photometry." Proceedings of the International Astronomical Union 8, S289 (2012): 74–81. http://dx.doi.org/10.1017/s174392131202114x.

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AbstractIn determining the distances to stars within the Milky Way galaxy, one often uses photometric or spectroscopic parallaxes. In these methods, the type of each individual star is determined, and the absolute magnitude of that star type is compared with the measured apparent magnitude to determine individual distances. In this paper, we define the term statistical photometric parallax, in which statistical knowledge of the absolute magnitudes of stellar populations is used to determine the underlying density distributions of those stars. This technique has been used to determine the densi

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Halbwachs, Jean–Louis. "First Double Star Observations in the HIPPARCOS Tycho Project." International Astronomical Union Colloquium 135 (1992): 429–34. http://dx.doi.org/10.1017/s0252921100006916.

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AbstractThe Tycho project will provide positions and (B, V) magnitudes for about 1 million stars, and will be complete for stars brighter than magnitude (B + V)/2 = 10.5. The components of double stars will obtain individual measurements when the separations are wider than 3″.

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Catelan, M. "The ages of (the oldest) stars." Proceedings of the International Astronomical Union 13, S334 (2017): 11–20. http://dx.doi.org/10.1017/s1743921318000868.

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AbstractMuch progress has been achieved in the age-dating of old stellar systems, and even of individual stars in the field, in the more than sixty years since the evolution of low-mass stars was first correctly described. In this paper, I provide an overview of some of the main methods that have been used in this context, and discuss some of the issues that still affect the determination of accurate ages for the oldest stars.

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Pavlovski, K., and J. Southworth. "Quantitative Spectroscopy of Close Binary Stars." Proceedings of the International Astronomical Union 7, S282 (2011): 359–64. http://dx.doi.org/10.1017/s1743921311027839.

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AbstractThe method of spectral disentangling has now created the opportunity for studying the chemical composition in previously inaccessible components of binary and multiple stars. This in turn makes it possible to trace their chemical evolution, a vital aspect in understanding the evolution of stellar systems. We review different ways to reconstruct individual spectra from eclipsing and non-eclipsing systems, and then concentrate on some recent applications to detached binaries with high-mass and intermediate-mass stars, and Algol-type mass-transfer systems.

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Dukov, E. V. "“Stars” from the Tube." Observatory of Culture, no. 3 (June 28, 2015): 28–36. http://dx.doi.org/10.25281/2072-3156-2015-0-3-28-36.

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“Stars” from the Tube (by Evgeny Dukov) deals with the new socio-cultural trend - individual artistic industry. It developed on the basis of appearance in the Internet of the Blog website (1990-s) and the YouTube video hosting (2000-s). Arisen independently of one another, they began to play a very important role in contemporary musical life: the bloggers became conductors of the new musical content that they would “catch” in the Internet; the technical capabilities of YouTube made saturation of that content simple, even for novice users. All this has led to the emergence of a new type of “sta

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32

Galli, P. A. B., R. Teixeira, C. Ducourant, and C. Bertout. "Kinematic distances of pre-main-sequence stars in the Lupus star-forming region." Proceedings of the International Astronomical Union 8, S289 (2012): 390–93. http://dx.doi.org/10.1017/s1743921312021783.

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AbstractTo reliably determine the main physical parameters (masses and ages) of young stars, we must know their distances. While the average distance to nearby star-forming regions (<300 pc) is often known, the distances to individual stars are usually unknown. Individual distances to members of young moving groups can be derived from their radial velocities and proper motions using the convergent-point strategy. We investigate the kinematic properties of the Lupus moving group with the primary objective of deriving individual distances to all group members.

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Kunder, Andrea. "RAVE-Gaia and the impact on Galactic archeology." Proceedings of the International Astronomical Union 12, S330 (2017): 176–80. http://dx.doi.org/10.1017/s1743921317006160.

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AbstractThe new data release (DR5) of the RAdial Velocity Experiment (RAVE) includes radial velocities of 520,781 spectra of 457,588 individual stars, of which 215,590 individual stars are released in the Tycho-Gaia astrometric solution (TGAS) in Gaia DR1. Therefore, RAVE contains the largest TGAS overlap of the recent and ongoing Milky Way spectroscopic surveys. Most of the RAVE stars also contain stellar parameters (effective temperature, surface gravity, overall metallicity), as well as individual abundances for Mg, Al, Si, Ca, Ti, Fe, and Ni. Combining RAVE with TGAS brings the uncertainti

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Treyer, Marie-A. "Massive stars in low-redshift galaxies." Symposium - International Astronomical Union 212 (2003): 663–70. http://dx.doi.org/10.1017/s0074180900213053.

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I summarize the method commonly used to estimate the current star formation rate per unit volume as a function of redshift from various star formation diagnostics, as well as the often conflicting results from the various multi-wavelength datasets collected in recent years. Combined together, and with the help of theoretical and empirical models, these results allow us to address the issues of excitation, reddening, metallicity, and star formation history in individual galaxies at low redshift. They seem to point to the fact, that a lot of the star formation in the local universe, and potentia

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Hirai, Yutaka, Michiko S. Fujii, and Takayuki R. Saitoh. "SIRIUS project. I. Star formation models for star-by-star simulations of star clusters and galaxy formation." Publications of the Astronomical Society of Japan 73, no. 4 (2021): 1036–56. http://dx.doi.org/10.1093/pasj/psab038.

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Abstract Most stars are formed as star clusters in galaxies, which then disperse into galactic disks. Upcoming exascale supercomputational facilities will enable simulations of galaxies and their formation by resolving individual stars (star-by-star simulations). This will substantially advance our understanding of star formation in galaxies, star cluster formation, and assembly histories of galaxies. In previous galaxy simulations, a simple stellar population approximation was used. It is, however, difficult to improve the mass resolution with this approximation. Therefore, a model for formin

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Noguchi, K., Z. Qian, J. Sun, G. Wang, J. Wang, and Y. Rao. "Space Distribution of Carbon Stars in Our Galaxy." Symposium - International Astronomical Union 177 (2000): 21–26. http://dx.doi.org/10.1017/s0074180900002205.

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We are attempting to investigate the space distribution of carbon stars in our Galaxy by evaluating the distances of individual carbon stars. We estimate the distance by evaluating the total radiant energy of each star and assuming a value for the bolometric magnitude of carbon stars. Since the flux maxima of carbon stars are mostly in the near-infrared (NIR), NIR photometric data are most useful for evaluating the total energy. We have compiled NIR photometric data for 694 carbon stars at all galactic longitudes and have made new observations of 470 carbon stars in the galactic longitude regi

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Beers, Timothy C., Deokkeun An, Jennifer A. Johnson, et al. "Metallicity Mapping with gri Photometry: The Virgo Overdensity and the Halos of the Galaxy." Proceedings of the International Astronomical Union 5, S262 (2009): 127–30. http://dx.doi.org/10.1017/s1743921310002644.

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AbstractWe describe the methodology required for estimation of photometric estimates of metallicity based on the SDSS gri passbands, which can be used to probe the properties of main-sequence stars beyond ~10 kpc, complementing studies of nearby stars from more metallicity-sensitive color indices that involve the u passband. As a first application of this approach, we determine photometric metal abundance estimates for individual main-sequence stars in the Virgo Overdensity, which covers almost 1000 deg2 on the sky, based on a calibration of the metallicity sensitivity of stellar isochrones in

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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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Sperauskas, J., V. Deveikis, and A. Tokovinin. "Spectroscopic orbits of nearby stars." Astronomy & Astrophysics 626 (June 2019): A31. http://dx.doi.org/10.1051/0004-6361/201935346.

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Aims. We observed stars with variable radial velocities to determine their spectroscopic orbits. Methods. Velocities are presented of 132 targets taken over a time span reaching 30 years. These were measured with the correlation radial velocity spectrometers (1917 velocities) and the new VUES echelle spectrograph (627 velocities), with a typical accuracy of 0.5 and 0.2 km s−1, respectively. Results. We derived spectroscopic orbits of 57 stars (including 53 first-time orbits), mostly nearby dwarfs of spectral types K and M, with some being HIPPARCOS astrometric binaries. Their periods range fro

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A. Bernstein, Rebecca, and Andrew McWilliam. "A New Method for Measuring the Detailed Chemical Composition of Globular Clusters from High-Resolution, Integrated-Light Spectra." Symposium - International Astronomical Union 207 (2002): 739–42. http://dx.doi.org/10.1017/s007418090022473x.

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We are developing a method for measuring the detailed chemical composition and evolutionary history of extragalactic star clusters from high resolution spectra of their integrated light as one would from spectra of individual stars. In this paper, we show high signal-to-noise ratio echelle spectra of the integrated light of two Galactic globular clusters and equivalent-quality spectra of individual stars in those clusters in order to briefly illustrate some subtleties of the analysis method.

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Galli, P. A. B., C. Bertout, R. Teixeira, and C. Ducourant. "T Tauri Disk Lifetime in the Lupus Association." Proceedings of the International Astronomical Union 10, S314 (2015): 191–92. http://dx.doi.org/10.1017/s1743921315006262.

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AbstractIn a recent study, we derived individual distances for a sample of pre-main sequence stars that define the comoving association of young stars in the Lupus star-forming region. Here, we use these new distances to investigate the mass and age distributions of Lupus T Tauri stars and derive the average disk lifetime in the Lupus association based on an empirical disk model.

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Morgan, S. "WWW Archive of Fourier Coefficients." International Astronomical Union Colloquium 185 (2002): 168–69. http://dx.doi.org/10.1017/s0252921100015918.

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AbstractFourier coefficients are a valuable tool in the study of a wide variety of pulsating stars. They can be used to derive various physical parameters, including mass, luminosity, metallicity and effective temperature and are frequently used to discriminate between different pulsation modes. With the increase in large-scale surveys and the availability of data on the Internet, the number of Fourier coefficients available for study has expanded greatly and it is difficult to find all current data for individual stars or a subset of stars. To assist others in obtaining and making use of Four

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Kvíz, Z. "Phase-night diagram for periodic variable stars." Symposium - International Astronomical Union 118 (1986): 297–98. http://dx.doi.org/10.1017/s0074180900151587.

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A program has been developed for the Hewlett-Packard Computer 9845 to represent in a graphical form the period of observability, for individual nights, of periodic phenomena of stars with respect to the phase. One version of the program (Fig. 1) gives the observability with respect to the phase for the whole year. The other version (Fig. 2) gives the beginning and end of the suitable observing interval for several observatories around the world thus facilitating preparation of a program for 24-hour continuous observation.

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Kniazev, Alexei A., and Simon A. Pustilnik. "ELTs and the study of individual, massive stars typical of “primordial” galaxies." Proceedings of the International Astronomical Union 1, S232 (2005): 306–7. http://dx.doi.org/10.1017/s1743921306000780.

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Roberts, Jr., Lewis C. "Three Methods of Determining Magnitudes of Individual Stars in Resolved Binary Systems." Publications of the Astronomical Society of the Pacific 111, no. 759 (1999): 650. http://dx.doi.org/10.1086/316358.

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Trust, Otto, Edward Jurua, Peter De Cat, Santosh Joshi, and Patricia Lampens. "HERMES spectroscopy of normal A and Am stars." Monthly Notices of the Royal Astronomical Society 504, no. 4 (2021): 5528–42. http://dx.doi.org/10.1093/mnras/stab1149.

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ABSTRACT The nominal Kepler mission provided very high precision photometric data. Using these data, interesting phenomena such as spots, and ‘hump and spike’ features were observed in the light curves of some normal A and metallic lined A stars (Am stars). However, the connection between such phenomena and the chemical peculiarity of the Am stars is still unclear. In order to make progress on these issues, it's important to collect high-resolution spectroscopic data to determine their fundamental parameters and individual chemical abundances. In this paper, we present a spectroscopic study of

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Hamann, W. R., and L. Koesterke. "Spectral Analyses of WC-Type Central Stars." Symposium - International Astronomical Union 155 (1993): 87. http://dx.doi.org/10.1017/s0074180900170172.

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Models have been developed in Kiel for massive (Pop. I) WR stars which account for multi-level non-LTE radiation transfer in spherically expanding atmospheres. The published (Koesterke et al. 1992) grid of models for WC composition (40% helium, 60% carbon by mass) can be applied to low-mass stars as well by means of the scaling properties of WR spectra (Hamann et al. 1992) and allow a rough guess of the parameters, while individual calculations are necessary for a detailed analysis and the determination of the chemical composition.

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Breger, Michel. "Asteroseismology of δ Scuti Stars: Observations". Symposium - International Astronomical Union 185 (1998): 323–30. http://dx.doi.org/10.1017/s0074180900238898.

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We review recent observational developments which provide important asteroseismological tools. Extensive multisite campaigns of individual δ Scuti stars show that 24 or more pulsation modes with ℓ = 0 to 2 can be detected photometrically. Spectroscopically, also about 30 modes have been detected, and these can be identified with modes of ℓ values up to 20. Since each technique favors the detection of specific types of modes, hundreds or thousands of modes must be excited in δ Scuti stars.We examine the quantities which can be matched between observations and theoretical models specifically com

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Adibekyan, V., S. G. Sousa, N. C. Santos, et al. "Benchmark stars, benchmark spectrographs." Astronomy & Astrophysics 642 (October 2020): A182. http://dx.doi.org/10.1051/0004-6361/202038793.

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Context. Gaia benchmark stars are selected to be calibration stars for different spectroscopic surveys. Very high-quality and homogeneous spectroscopic data for these stars are therefore required. We collected ultrahigh-resolution ESPRESSO spectra for 30 of the 34 Gaia benchmark stars and made them public. Aims. We quantify the consistency of the results that are obtained with different high- (R ~ 115 000), and ultrahigh- (R ~ 220 000) resolution spectrographs. We also comprehensively studied the effect of using different spectral reduction products of ESPRESSO on the final spectroscopic resul

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Rameau, Julien, Gaël Chauvin, Anne-Marie Lagrange, Philippe Delorme, and Justine Lannier. "Giant planets around AF and M stars." Proceedings of the International Astronomical Union 8, S299 (2013): 64–65. http://dx.doi.org/10.1017/s1743921313007898.

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AbstractWe present the results of two three-year surveys of young and nearby stars to search for wide orbit giant planets. On the one hand, we focus on early-type and massive, namely β Pictoris analogs. On the other hand, we observe late type and very low mass stars, i.e., M dwarfs. We report individual detections of new planetary mass objects. According to our deep detection performances, we derive the observed frequency of giant planets between these two classes of parent stars. We find frequency between 6 to 12% but we are not able to assess a/no correlation with the host-mass.

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