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Academic literature on the topic 'Stars'

Author: Grafiati

Published: 4 June 2021

Last updated: 22 February 2025

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Journal articles on the topic "Stars"

1

Swann, Brian. "Stars Stars Stars." College English 57, no. 2 (February 1995): 196. http://dx.doi.org/10.2307/378810.

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Jacke, Christoph. "Stars, Anti-Stars, Anti-Star-Stars." Persona Studies 10, no. 1 (May 1, 2024): 56–73. http://dx.doi.org/10.21153/psj2024vol10no1art1872.

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The phenomenon of stars and celebrities in media cultures – and especially in popular music cultures – seems to be omnipresent. At the same time, there is an astounding lack of analysis and research on these media personalities and personas, and international celebrity studies only recently a developing new field. Similarly, these kinds of observations are still very rare especially in German sociology as well as communication, media, culture and popular music studies. In this article, I therefore want to concentrate on the foundations of studying stars and celebrities within the attention economies by undertaking a theoretical transmedia-cultural framing of media personas and suggesting a typology. This ensuing typology of stars, anti-stars, and anti-star stars – especially within popular music cultures – demonstrates how stars and celebrities and their quantities and qualities of success and peer-group specific values coming form programs of (media and music) culture can serve as persona-seismographs of socio-cultural change between tradition and innovation.

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Østgaard, Erlend. "Compact stars: Neutron stars or quark stars or hybrid stars?" Physics Reports 242, no. 4-6 (July 1994): 313–32. http://dx.doi.org/10.1016/0370-1573(94)90166-x.

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JAIKUMAR, P., C. GALE, D. PAGE, and M. PRAKASH. "DISTINGUISHING BARE QUARK STARS FROM NEUTRON STARS." International Journal of Modern Physics A 19, no. 31 (December 20, 2004): 5335–42. http://dx.doi.org/10.1142/s0217751x04022566.

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Observations to date cannot distinguish neutron stars from self-bound bare quark stars on the basis of their gross physical properties such as their masses and radii alone. However, their surface luminosity and spectral characteristics can be significantly different. Unlike a normal neutron star, a bare quark star can emit photons from its surface at super-Eddington luminosities for an extended period of time. We present a calculation of the photon bremsstrahlung rate from the bare quark star's surface, and indicate improvements that are required for a complete characterization of the spectrum. The observation of this distinctive photon spectrum would constitute an unmistakable signature of a strange quark star and shed light on color superconductivity at stellar densities.

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Dimitrijević, Milan S. "Stark broadening of stellar Pt II lines." Symposium - International Astronomical Union 162 (1994): 337–38. http://dx.doi.org/10.1017/s0074180900215258.

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Lines of Pt II have been discovered in Hg Mn stars by Dworetsky (1969). The analysis of a few strong Pt II transitions, which are also observed in IUE spectra of stars, has shown (Dworetsky et al., 1984) “that Pt is, like Hg, among the most overabundant elements in the atmospheres of Hg Mn stars, with enhancements of the order of 104 to 105 over the solar system abundances”. Dworetsky et al. (1984) selected also the four Pt II lines which might be used for astrophysical applications. Moreover, they determined the corresponding theoretical gf values. The aim of this contribution is to investigate the Stark broadening of these Pt II lines and to provide the corresponding Stark widths.

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Grassi, F. "Quark core stars, quark stars and strange stars." Zeitschrift f�r Physik C Particles and Fields 44, no. 1 (March 1989): 129–38. http://dx.doi.org/10.1007/bf01548591.

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Folsom, C. P., S. Bagnulo, G. A. Wade, J. D. Landstreet, and E. Alecian. "Chemical peculiarities in magnetic and non-magnetic pre-main sequence A and B stars." Proceedings of the International Astronomical Union 9, S302 (August 2013): 87–90. http://dx.doi.org/10.1017/s1743921314001781.

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AbstractIn A- and late B-type stars, strong magnetic fields are always associated with Ap and Bp chemical peculiarities. However, it is not clear at what point in a star's evolution those peculiarities develop. Strong magnetic fields have been observed in pre-main sequence A and B stars (Herbig Ae and Be stars), and these objects have been proposed to be the progenitors of Ap and Bp stars. However, the photospheric chemical abundances of these magnetic Herbig stars have not been studied carefully, and furthermore the chemical abundances of 'normal' non-magnetic Herbig stars remain poorly characterized. To investigate this issue, we have studied the photospheric compositions of 23 Herbig stars, four of which have confirmed magnetic fields. Surprisingly, we found that half the non-magnetic stars in our sample show λ Bootis chemical peculiarities to varying degrees. For the stars with detected magnetic fields, we find one chemically normal star, one star with λ Boo peculiarities, one star displaying weak Ap/Bp peculiarities, and one somewhat more evolved star with somewhat stronger Ap/Bp peculiarities. These results suggests that Ap/Bp peculiarities are preceded by magnetic fields, and that these peculiarities develop over the pre-main sequence lives of A and B stars. The incidence of λ Boo stars we find is much higher than that seen on the main sequence. We argue that a selective accretion model for the formation of λ Boo peculiarities is a natural explanation for this remarkably large incidence.

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Vickers, J. J., A. P. Huxor, and E. K. Grebel. "Blue Horizontal Branch Stars in Pan-STARRS." EAS Publications Series 67-68 (2014): 183–86. http://dx.doi.org/10.1051/eas/1567032.

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Bagnulo, S. "Statistical Properties of Magnetic CP Stars." Symposium - International Astronomical Union 210 (2003): 209–20. http://dx.doi.org/10.1017/s0074180900133376.

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Magnetic fields of chemically peculiar (CP) stars of the upper main sequence are characterised by a geometry organised at a large scale, permeating the entire photosphere, and with a typical strength of the order of 0.1–30 kG. Here I review the results obtained from statistical studies of the structures of the magnetic fields of CP stars, which are aimed at finding how magnetic strength and morphology are correlated with other stellar characteristics and with the star's evolutionary state.

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Gondek, Dorota. "Neutron stars and strange stars." International Astronomical Union Colloquium 160 (1996): 133–34. http://dx.doi.org/10.1017/s0252921100041282.

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If strange quark plasma is the real ground state of baryonic matter (Witten 1984), then some of neutron stars (NS) could actually be strange stars (SS). It is difficult to distinguish SS from NS observationally. They have similar radii and masses and their crusts are built of the same matter. It seems that a good method for testing the existence of SS would be the studies of phenomena related to the stellar pulsations. In 1976 Boriakoff proposed that radial oscillations of NS could be observed within radio subpulses of pulsars. While various modes of pulsations of NS were studied by a number of authors, little attention was paid to seismological signatures of SS. The radial oscilations of bare SS were studied by Väth & Chanmugam (1992). Recently Weber (this volume) studied properties of stars made of matter described by BPS equation of state (EOS) (Baym et al. 1971) with a ball of strange matter inside, but they mainly concentrated on stability of white-dwarf-like SS. In this work I present fully relativistic calculations of the radial oscillation frequencies of SS. I determined the fundamental frequency for bare SS and SS with two different types of crusts depending on origin (Alcock et al. 1986) of SS and showed differences between them.

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Dissertations / Theses on the topic "Stars"

1

Moeckel, Nickolas Barry. "Massive stars, disks, and clustered star formation." Connect to online resource, 2008. http://gateway.proquest.com/openurl?url_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:dissertation&res_dat=xri:pqdiss&rft_dat=xri:pqdiss:3303877.

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Belles, Pierre-Emmanuel Aime Marcel. "Formation of stars and star clusters in colliding galaxies." Thesis, University of Hertfordshire, 2013. http://hdl.handle.net/2299/10312.

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Mergers are known to be essential in the formation of large scale structures and to have a significant role in the history of galaxy formation and evolution. Besides a morphological transformation, mergers induce important bursts of star formation. These starburst are characterised by high Star Formation Efficiencies (SFEs) and Specific Star Formation Rates, i.e., high Star Formation Rates (SFR) per unit of gas mass and high SFR per unit of stellar mass, respectively, compared to spiral galaxies. At all redshifts, starburst galaxies are outliers of the sequence of star-forming galaxies defined by spiral galaxies. We have investigated the origin of the starburst-mode of star formation, in three local interacting systems: Arp 245, Arp 105 and NGC7252. We combined high-resolution JVLA observations of the 21-cm line, tracing the Hi diffuse gas, with UV GALEX observations, tracing the young star-forming regions. We probe the local physical conditions of the Inter- Stellar Medium (ISM) for independent star-forming regions and explore the atomic-to-dense gas transformation in different environments. The SFR/H i ratio is found to be much higher in central regions, compared to outer regions, showing a higher dense gas fraction (or lower Hi gas fraction) in these regions. In the outer regions of the systems, i.e., the tidal tails, where the gas phase is mostly atomic, we find SFR/H i ratios higher than in standard Hi-dominated environments, i.e., outer discs of spiral galaxies and dwarf galaxies. Thus, our analysis reveals that the outer regions of mergers are characterised by high SFEs, compared to the standard mode of star formation. The observation of high dense gas fractions in interacting systems is consistent with the predictions of numerical simulations; it results from the increase of the gas turbulence during a merger. The merger is likely to affect the star-forming properties of the system at all spatial scales, from large scales, with a globally enhanced turbulence, to small scales, with possible modifications of the initial mass function. From a high-resolution numerical simulation of the major merger of two spiral galaxies, we analyse the effects of the galaxy interaction on the star forming properties of the ISM at the scale of star clusters. The increase of the gas turbulence is likely able to explain the formation of Super Star Clusters in the system. Our investigation of the SFR–H i relation in galaxy mergers will be complemented by highresolution Hi data for additional systems, and pushed to yet smaller spatial scales.

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Davey, Stephen. "Irradiation of the secondary star in cataclysmic variable stars." Thesis, University of Sussex, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.386388.

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Souto, D., K. Cunha, D. A. Garcia-Hernandez, O. Zamora, C. Allende Prieto, V. V. Smith, S. Mahadevan, et al. "Chemical Abundances of M-Dwarfs from the Apogee Survey. I. The Exoplanet Hosting Stars Kepler-138 and Kepler-186." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624381.

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We report the first detailed chemical abundance analysis of the exoplanet-hosting M-dwarf stars Kepler-138 and Kepler-186 from the analysis of high-resolution (R similar to 22,500) H-band spectra from the SDSS-IV-APOGEE survey. Chemical abundances of 13 elements-C, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, and Fe-are extracted from the APOGEE spectra of these early M-dwarfs via spectrum syntheses computed with an improved line list that takes into account H2O and FeH lines. This paper demonstrates that APOGEE spectra can be analyzed to determine detailed chemical compositions of M-dwarfs. Both exoplanet-hosting M-dwarfs display modest sub-solar metallicities: [Fe/H](Kepler-138) = -0.09 +/- 0.09 dex and [Fe/H](Kepler-186) = -0.08 +/- 0.10 dex. The measured metallicities resulting from this high-resolution analysis are found to be higher by similar to 0.1-0.2 dex than previous estimates from lower-resolution spectra. The C/O ratios obtained for the two planet-hosting stars are near-solar, with values of 0.55 +/- 0.10 for Kepler-138 and 0.52 +/- 0.12 for Kepler-186. Kepler-186 exhibits a marginally enhanced [Si/Fe] ratio.

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Johnston, Katharine G. "Observational signatures of massive star formation : an investigation of the environments in which they form, and the applicability of the paradigm of low-mass star formation." Thesis, University of St Andrews, 2011. http://hdl.handle.net/10023/1895.

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This thesis presents both a study of the cluster-scale environments in which massive stars form, investigating in particular how the ionized gas in these regions relates to the molecular star-forming material, as well as detailed studies of two luminous forming stars, AFGL 2591 and IRAS 20126+4104, to determine whether they are forming similarly to their low-mass counterparts. The results of this work include the identification of 35 HII regions (20 newly discovered) via a radio continuum survey of ionized gas towards 31 molecular cluster-forming clumps. The observed ionized gas was found to be preferentially associated with the clumps, which were shown to have a range of evolutionary stages. The massive star formation efficiency was determined for the clumps with associated ionized gas, and a relationship was found between the mass of the clumps and the mass of their embedded massive stars. By modelling the SEDs and images of AFGL 2591 and IRAS 20126+4104, it was found that the geometry of their circumstellar material was generally consistent with an envelope plus disk, similar to that expected for low-mass protostars. However, within the central ~1800 AU, the mid-IR images of IRAS 20126+4104 were better described by only a flattened envelope, suggesting that the radiation from IRAS 20126+4104 may be affecting the regions closest to the star. Observations of the ionized and molecular gas towards AFGL 2591 were carried out, and a photoionization code was developed to interpret these observations. The results showed that the observed 3.6 cm emission is likely to be produced by both a shock-ionized jet and a hypercompact HII region that does not appear to have disrupted the jet or the large-scale circumstellar environment. In addition, the C¹⁸O(1-0) emission observed towards AFGL2591 traces the densest parts of the outflow, with the blue-shifted emission exhibiting many of the properties of the outflows from low-mass protostars.

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Telleschi, Alessandra Silvia. "Coronal evolution of solar-like stars : X-ray spectroscopy of stars in star-forming regions and the solar neighborhood /." Zürich : ETH, 2007. http://e-collection.ethbib.ethz.ch/show?type=diss&nr=17018.

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Nelmes, Susan Grace. "Skyrmion stars." Thesis, Durham University, 2012. http://etheses.dur.ac.uk/5258/.

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Neutron stars are very dense stars composed almost entirely of neutrons. As such, they should be able to be described by Quantum Chromodynamics (QCD). As QCD is a very complicated theory from which it is difficult to produce quantitative results we rely on effective theories to describe QCD physics. It has previously been shown that the Skyrme model, which has topological soliton solutions that can be identified as baryons, is such a low energy effective field theory for QCD. In this thesis, after presenting background material in chapters 1, 2 and 3, we explore the results of attempting to use the theory proposed by Skyrme to model neutron stars by investigating two models. The first, discussed in chapter 4 and based on original research, considers rational map ansatz solutions to the Skyrme model. By coupling the model using this ansatz to gravity and introducing a new way of stacking together the shell-like solutions that form we find minimum energy configurations that are stable models of neutron stars. They are, however, slightly too small to be considered a good model so a second approach is tried. The second model considers Skyrme crystal configurations. By using a relation between the energy per baryon of a Skyrme crystal and its anisotropic deformations we are able to find two equations of state for the crystal. These are combined with a Tolman-Oppenheimer-Volkoff equation, generalised to describe anisotropic deformations, to model neutron stars. We find that below a critical mass all deformations are isotropic and above it they are anisotropic up to a particular maximum mass and that this approach compares well with experimental observations. This second model is described in chapter 5 and is based on original research.

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Celizic, Joseph S. "Beyond Stars." Bowling Green State University / OhioLINK, 2009. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1243878273.

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Grigg, Madeline J. "Dog Stars." Bowling Green State University / OhioLINK, 2019. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1555682074446507.

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Frink, Sabine. "Kinematics of T Tauri stars in nearby star forming regions." [S.l. : s.n.], 1999. http://deposit.ddb.de/cgi-bin/dokserv?idn=961689390.

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Books on the topic "Stars"

1

Wentworth, K. D. Stars over stars. Riverdale, N.Y: Baen, 2001.

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translator, Zhang Xiangdong, ed. Xing! Xing! Xing!: Stars! Stars! Stars! 2nd ed. Wuhan: Chang Jiang shao nian er tong chu ban she, 2014.

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Simon, Seymour, and Seymour Simon. Stars. New York: Morrow, 1986.

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Davis, Dresser. Stars. New York, USA: Random House Value Publishing, 1987.

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Birch, Robin. Stars. New York, NY: Chelsea Clubhouse, 2008.

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Sabin, Louis. Stars. Mahwah, N.J: Troll Associates, 1985.

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Wandelmaier, Roy. Stars. Mahwah, N.J: Troll Associates, 1985.

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Harvey, Kathryn. Stars. Nashville, TN: Turner Pub. Co., 2012.

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Michael, George. Stars. Mankato, Minn: Creative Education, Inc., 1991.

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Simon, Seymour. Stars. New York: Morrow, 1986.

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Book chapters on the topic "Stars"

1

van Zyl, J. E. "Stars and Double Stars." In Unveiling the Universe, 157–93. London: Springer London, 1996. http://dx.doi.org/10.1007/978-1-4471-1037-8_10.

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Harwit, Martin. "Stars." In Astrophysical Concepts, 303–73. New York, NY: Springer New York, 1988. http://dx.doi.org/10.1007/978-1-4757-2019-8_8.

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Bartholomew, P., and Sarah Vinson. "STARS." In Software Systems for Structural Optimization, 251–83. Basel: Birkhäuser Basel, 1993. http://dx.doi.org/10.1007/978-3-0348-8553-9_13.

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Eggenberger, Patrick, and Sylvia Ekström. "Stars." In Encyclopedia of Astrobiology, 1574. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-11274-4_1503.

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Harwit, Martin. "Stars." In Astrophysical Concepts, 287–349. New York, NY: Springer New York, 1998. http://dx.doi.org/10.1007/978-1-4757-2928-3_8.

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Inglis, Michael David. "Stars." In Field Guide to the Deep Sky Objects, 23–114. London: Springer London, 2001. http://dx.doi.org/10.1007/978-1-4471-3680-4_2.

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Etherington-Wright, Christine, and Ruth Doughty. "Stars." In Understanding Film Theory, 213–31. London: Macmillan Education UK, 2011. http://dx.doi.org/10.1007/978-0-230-34392-4_14.

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Chruściel, Piotr T. "Stars." In Compact Textbooks in Mathematics, 167–87. Cham: Springer International Publishing, 2019. http://dx.doi.org/10.1007/978-3-030-28416-9_5.

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Meisenheimer, Wolfgang. "Stars." In Modelle als Denkräume, Beispiele und Ebenbilder, 142–45. Wiesbaden: Springer Fachmedien Wiesbaden, 2018. http://dx.doi.org/10.1007/978-3-658-20115-9_30.

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Böhme, S., Walter Fricke, H. Hefele, Inge Heinrich, W. Hofmann, D. Krahn, V. R. Matas, Lutz D. Schmadel, and G. Zech. "Stars." In Literature 1984, Part 2, 456–569. Berlin, Heidelberg: Springer Berlin Heidelberg, 1985. http://dx.doi.org/10.1007/978-3-662-12346-1_13.

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Conference papers on the topic "Stars"

1

WEBER, FRIDOLIN. "NEUTRON STARS AND QUARK STARS." In Proceedings of the KIAS–APCTP International Symposium on Astro-Hadron Physics. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812702524_0010.

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Masseron, Thomas. "Stellar Nucleosynthesis in the Galactic History: the Carbon Stars." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905535.

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Fan, Xiaohui. "Observational Constraints of the End of Cosmic Reionization." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905658.

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Yoshida, Naoki. "Simulating the Formation of Primordial Proto‐Stars." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905546.

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Kashlinsky, A. "Cosmic Infrared Background from Early Epochs: Searching for Signatures of the First Stars." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905518.

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Thompson, Rodger I. "The Near Infrared Background: Resolved and Identified." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905519.

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Fernandez, Elizabeth R., and Eiichiro Komatsu. "The Cosmic Near Infrared Background: Remnant Light From Early Stars." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905520.

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Iocco, Fabio. "High Energy Neutrino Signals from the First Stars." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905521.

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Joggerst, Candace Church, Alexander Heger, and Stanford E. Woosley. "Multidimensional Simulations of Mixing in Zero‐ and Solar‐Metallicity SNe." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905557.

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Glover, Simon. "Chemistry and Cooling in Metal‐Free and Metal‐Poor Gas." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905558.

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Reports on the topic "Stars"

1

Grassi, F. Quark core stars, quark stars and strange stars. Office of Scientific and Technical Information (OSTI), January 1988. http://dx.doi.org/10.2172/5237159.

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Gutiérrez, Germán, and Thomas Philippon. Fading Stars. Cambridge, MA: National Bureau of Economic Research, February 2019. http://dx.doi.org/10.3386/w25529.

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Agrawal, Ajay, John McHale, and Alex Oettl. Why Stars Matter. Cambridge, MA: National Bureau of Economic Research, March 2014. http://dx.doi.org/10.3386/w20012.

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Ekman, R. STARS Reusability Guidelines. Fort Belvoir, VA: Defense Technical Information Center, April 1990. http://dx.doi.org/10.21236/ada228468.

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Eggleton, P. Magnetic Dynamos and Stars. Office of Scientific and Technical Information (OSTI), February 2007. http://dx.doi.org/10.2172/1036872.

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Ekman, R. IBM STARS Repository Guidebook. Fort Belvoir, VA: Defense Technical Information Center, April 1990. http://dx.doi.org/10.21236/ada228470.

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Smullen, Rachel. We are made of star stuff: How stars (and planets) are created. Office of Scientific and Technical Information (OSTI), November 2021. http://dx.doi.org/10.2172/1833240.

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Tekesky, Robert S. Joint STARS RTMM Carrying Case. Fort Belvoir, VA: Defense Technical Information Center, January 1996. http://dx.doi.org/10.21236/ada304544.

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McDonald, Catherine W., and Teresa L. Anderson. STARS Repository Bibliography Version 1.1. Fort Belvoir, VA: Defense Technical Information Center, January 1988. http://dx.doi.org/10.21236/ada227597.

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McDonald, Catherine W. STARS Repository Guidebook Version 1.2. Fort Belvoir, VA: Defense Technical Information Center, April 1988. http://dx.doi.org/10.21236/ada227598.

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