Relevant bibliographies by topics / White dwarf stars Spectra

Academic literature on the topic 'White dwarf stars Spectra'

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Published: 10 December 2022
Last updated: 28 January 2023

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Journal articles on the topic "White dwarf stars Spectra"

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Kepler, S. O., Alejandra Daniela Romero, Ingrid Pelisoli, and Gustavo Ourique. "White Dwarf Stars." International Journal of Modern Physics: Conference Series 45 (January 2017): 1760023. http://dx.doi.org/10.1142/s2010194517600230.

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White dwarf stars are the final stage of most stars, born single or in multiple systems. We discuss the identification, magnetic fields, and mass distribution for white dwarfs detected from spectra obtained by the Sloan Digital Sky Survey up to Data Release 13 in 2016, which lead to the increase in the number of spectroscopically identified white dwarf stars from 5[Formula: see text]000 to 39[Formula: see text]000. This number includes only white dwarf stars with [Formula: see text], i.e., excluding the Extremely Low Mass white dwarfs, which are necessarily the byproduct of stellar interaction.
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Shipman, H. L. "Variable white dwarfs." Proceedings of the International Astronomical Union 15, S357 (October 2019): 107–9. http://dx.doi.org/10.1017/s1743921320001386.

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AbstractAsteroseismology of white dwarf stars has led to a number of interesting results pertaining to the long term evolution and present state of white dwarf interiors. I will review recent results and will give a not necessarily comprehensive view of the prospects for further progress in this area. Two – but only two white dwarf stars - have shown the expected cooling as they age. Careful observations of a few white dwarfs with rich pulsational properties reveal interior compositions as well as the thickness of their surface layers. A few very well observed stars have revealed changes in their pulsational spectra which we don’t understand yet.
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Kepler, S. O., Ingrid Pelisoli, Detlev Koester, Nicole Reindl, Stephan Geier, Alejandra D. Romero, Gustavo Ourique, Cristiane de Paula Oliveira, and Larissa A. Amaral. "White dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 14." Monthly Notices of the Royal Astronomical Society 486, no. 2 (April 8, 2019): 2169–83. http://dx.doi.org/10.1093/mnras/stz960.

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ABSTRACT White dwarfs carry information on the structure and evolution of the Galaxy, especially through their luminosity function and initial-to-final mass relation. Very cool white dwarfs provide insight into the early ages of each population. Examining the spectra of all stars with 3σ proper motion in the Sloan Digital Sky Survey Data Release 14, we report the classification for 20 088 spectroscopically confirmed white dwarfs, plus 415 hot subdwarfs, and 311 cataclysmic variables. We obtain Teff, log g, and mass for hydrogen atmosphere white dwarf stars (DAs), warm helium atmosphere white dwarfs (DBs), hot subdwarfs (sdBs and sdOs), and estimate photometric Teff for white dwarf stars with continuum spectra (DCs). We find 15 793 sdAs and 447 dCs between the white dwarf cooling sequence and the main sequence, especially below $T_\mathrm{eff}\simeq 10\, 000$ K; most are likely low-mass metal-poor main-sequence stars, but some could be the result of interacting binary evolution.
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Hogg, M. A., S. L. Casewell, G. A. Wynn, E. S. Longstaff, I. P. Braker, M. R. Burleigh, R. H. Tilbrook, et al. "Confirming new white dwarf-ultracool dwarf binary candidates." Monthly Notices of the Royal Astronomical Society 498, no. 1 (August 10, 2020): 12–24. http://dx.doi.org/10.1093/mnras/staa2233.

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ABSTRACT We present the results of a study to discover prospective new white dwarf-L dwarf binaries as identified by their near-infrared excesses in the UKIDSS catalogue. We obtained optical spectra to validate the white dwarf nature for 22 of the candidate primary stars, confirming ten as white dwarfs and determining their effective temperatures and gravities. For all 10 white dwarfs, we determined that the near-infrared excess was indeed indicative of a cool companion. Six of these are suggestive of late M dwarf companions, and three are candidate L dwarf companions, with one straddling the M−L boundary. We also present near-infrared spectra of eight additional candidate white dwarf-ultracool dwarf binaries, where the white dwarf primary had been previously confirmed. These spectra indicate one candidate at the M−L boundary, three potential L dwarf companions, and one suspected M dwarf, which showed photometric variability on a ∼6 h period, suggesting the system may be close. Radial velocity follow-up is required to confirm whether these systems are close, or widely separated.
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Kepler, S. O., Detlev Koester, Ingrid Pelisoli, Alejandra D. Romero, and Gustavo Ourique. "White dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 16." Monthly Notices of the Royal Astronomical Society 507, no. 3 (August 24, 2021): 4646–60. http://dx.doi.org/10.1093/mnras/stab2411.

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ABSTRACT White dwarfs are the end state of the evolution of more than 97 per cent of all stars, and therefore carry information on the structure and evolution of the Galaxy through their luminosity function and initial-to-final mass relation. Examining the new spectra of all white or blue stars in the Sloan Digital Sky Survey Data Release 16, we report the spectral classification of 2410 stars, down to our identification cut-off of signal-to-noise ratio equal to three. We newly identify 1404 DAs, 189 DZs, 103 DCs, 12 DBs, and nine CVs. The remaining objects are a mix of carbon or L stars (dC/L), narrow-lined hydrogen-dominated stars (sdA), dwarf F stars, and P Cyg objects. As white dwarf stars were not targeted by SDSS DR16, the number of new discoveries is much smaller than in previous releases. We also report atmospheric parameters and masses for a subset consisting of 555 new DAs, 10 new DBs, and 85 DZs for spectra with signal-to-noise ratio larger than 10.
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Solheim, J. E. "Interacting Binary White Dwarf Stars." Symposium - International Astronomical Union 151 (1992): 461–64. http://dx.doi.org/10.1017/s0074180900122727.

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This group of stars consists of 4 systems, also called helium cataclysmics. Three of them show photometric variations and have been studied by the Whole Earth Telescope (WET), which have revealed multiperiodic light curves showing the signature of g-mode non-radial pulsations on the accreting star. The combination of accretion and g-mode pulsations gives a unique opportunity to test models for the accreator's structural changes in response to accretion. IUE-spectra provide additional physical parameters.
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Finch, Nicolle L., S. P. Preval, M. A. Barstow, S. L. Casewell, T. Ayres, B. Welsh, M. Bainbridge, and N. Reindl. "What can ISM and non-photospheric highly ionised lines in white dwarf spectra reveal about the β CMa tunnel?" Proceedings of the International Astronomical Union 15, S357 (October 2019): 220–24. http://dx.doi.org/10.1017/s1743921320001374.

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AbstractWhite dwarfs are useful objects with which to study the local interstellar medium (ISM). High ionisation state absorption features that cannot be attributed to the photosphere or the ISM have been observed along the line-of-sight to a number of white dwarf stars. Suggested origins of these lines include ionisation from past supernovae, stellar winds, circumstellar disks, photoionisation from nearby hot stars or also from the white dwarf itself. In this study we consider the origin of these non-photospheric highly ionised lines in two stars towards a rarefied region of the galaxy known as the extended β CMa Tunnel. We present preliminary results from our analysis of the first of these two stars.
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Fontaine, G., P. Brassard, P. Bergeron, and F. Wesemael. "White Dwarf Seismology at the Université de Montréal." International Astronomical Union Colloquium 139 (1993): 120. http://dx.doi.org/10.1017/s0252921100117063.

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Over the last several years, we have developed a comprehensive program aimed at better understanding the properties of pulsating DA white dwarfs (or ZZ Ceti stars). These stars are nonradial pulsators of the g-type, and their study can lead to inferences about their internal structure. For instance, the period spectrum of a white dwarf is most sensitive to its vertical chemical stratification, and one of the major goals of white dwarf seismology is to determine the thickness of the hydrogen layer that sits on top of a star. This can be done, in principle, by comparing in detail theoretical period spectra with the periods of the observed excited modes. Likewise, because the cooling rate of a white dwarf is very sensitive to the specific heat of its core material (and hence to its composition), it is possible to infer the core composition through measurements and interpretations of rates of period change in a pulsator.
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Allard, N. F., J. F. Kielkopf, S. Blouin, P. Dufour, F. X. Gadéa, T. Leininger, and G. Guillon. "Line shapes of the magnesium resonance lines in cool DZ white dwarf atmospheres." Astronomy & Astrophysics 619 (November 2018): A152. http://dx.doi.org/10.1051/0004-6361/201834067.

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Context. Line shapes of the magnesium resonance lines in white dwarf spectra are determined by the properties of magnesium atoms and the structure of the white dwarf atmosphere. Through their blanketing effect, these lines have a dominant influence on the model structure and thus on the determination from the spectra of other physical parameters that describe the stellar atmosphere and elemental abundances. Aims. In continuation of previous work on Mg+He lines in the UV, we present theoretical profiles of the resonance line of neutral Mg perturbed by He at the extreme density conditions found in the cool largely transparent atmosphere of DZ white dwarfs. Methods. We accurately determined the broadening of Mg by He in a unified theory of collisional line profiles using ab initio calculations of MgHe potential energies and transition matrix elements among the singlet electronic states that are involved for the observable spectral lines. Results. We computed the shapes and line parameters of the Mg lines and studied their dependence on helium densities and temperatures. We present results over the full range of temperatures from 4000 to 12 000 K needed for input to stellar spectra models. Atmosphere models were constructed for a range of effective temperatures and surface gravities typical for cool DZ white dwarfs. We present synthetic spectra tracing the behavior of the Mg resonance line profiles under the low temperatures and high gas pressures prevalent in these atmospheres. Conclusions. The determination of accurate opacity data of magnesium resonance lines together with an improved atmosphere model code lead to a good fit of cool DZ white dwarf stars. The broadening of spectral lines by helium needs to be understood to accurately determine the H/He and Mg/He abundance ratio in DZ white dwarf atmospheres. We emphasize that no free potential parameters or ad hoc adjustments were used to calculate the line profiles.
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Majlinger, Zlatko, Milan S. Dimitrijević, and Vladimir A. Srećković. "Stark broadening of Co ii spectral lines in hot stars and white dwarf spectra." Monthly Notices of the Royal Astronomical Society 496, no. 4 (July 9, 2020): 5584–90. http://dx.doi.org/10.1093/mnras/staa1947.

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ABSTRACT Stark full widths at half-maximum for 46 Co ii multiplets have been calculated using modified semi-empirical method. The obtained results have been used to demonstrate the importance of Stark broadening mechanism in DA and DB white dwarf and A star atmospheres. With the obtained results we also test possibility of using some approximate methods of Stark width calculations developed on the basis of regularities and systematic trends.
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Dissertations / Theses on the topic "White dwarf stars Spectra"

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Liebert, J., R. A. Saffer, and C. A. Pilachowski. "High Dispersion Observations of H alpha in the Suspected Brown Dwarf, White Dwarf Binary System G29-38." Steward Observatory, The University of Arizona (Tucson, Arizona), 1988. http://hdl.handle.net/10150/623899.

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We report on high dispersion spectroscopy of the Ha absorption line of the cool DA white dwarf G 29 -38. This is the star for which a recently detected infrared excess has been suggested to be due to a possible brown dwarf companion by Zuckerman and Becklin (1986, 1987). Three echelle spectra obtained at the Multiple Mirror Telescope and at the Kitt Peak Mayall 4m telescope in 1987 December show no evidence for radial velocity variations larger than -'1.1 ± 8.7 km s -1 and are used to derive a weighted heliocentric radial velocity Vr = 33.7 ± 4.3 km s -1 for the white dwarf. No emission component from the hypothesized secondary star is detected. These negative results do not constitute strong evidence against the companion hypothesis, since the expected orbital velocity of the white dwarf component could be quite small, and the companion's line emission could be too faint to be detected. However, the observation of a sharp absorption line core restricts the possible rotation of the white dwarf to < 40 km s -1 and ensures that any surface magnetic field has a strength < 105 gauss. These results make it unlikely that the DA white dwarf has previously been in a cataclysmic variable accretion phase.
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Bainbridge, Matthew, Martin Barstow, Nicole Reindl, W. Ü. Tchang-Brillet, Thomas Ayres, John Webb, John Barrow, et al. "Probing the Gravitational Dependence of the Fine-Structure Constant from Observations of White Dwarf Stars." MDPI AG, 2017. http://hdl.handle.net/10150/625061.

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Hot white dwarf stars are the ideal probe for a relationship between the fine-structure constant and strong gravitational fields, providing us with an opportunity for a direct observational test. We study a sample of hot white dwarf stars, combining far-UV spectroscopic observations, atomic physics, atmospheric modelling, and fundamental physics in the search for variation in the fine structure constant. This variation manifests as shifts in the observed wavelengths of absorption lines, such as quadruply ionized iron (FeV) and quadruply ionized nickel (NiV), when compared to laboratory wavelengths. Berengut et al. (Phys. Rev. Lett. 2013, 111, 010801) demonstrated the validity of such an analysis using high-resolution Space Telescope Imaging Spectrograph (STIS) spectra of G191-B2B. We have made three important improvements by: (a) using three new independent sets of laboratory wavelengths; (b) analysing a sample of objects; and (c) improving the methodology by incorporating robust techniques from previous studies towards quasars (the Many Multiplet method). A successful detection would be the first direct measurement of a gravitational field effect on a bare constant of nature. Here we describe our approach and present preliminary results from nine objects using both FeV and NiV.
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Levenhagen, Ronaldo S., Marcos P. Diaz, Paula R. T. Coelho, and Ivan Hubeny. "A Grid of Synthetic Spectra for Hot DA White Dwarfs and Its Application in Stellar Population Synthesis." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624926.

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In this work we present a grid of LTE and non-LTE synthetic spectra of hot DA white dwarfs (WDs). In addition to its usefulness for the determination of fundamental stellar parameters of isolated WDs and in binaries, this grid will be of interest for the construction of theoretical libraries for stellar studies from integrated light. The spectral grid covers both a wide temperature and gravity range, with 17,000 K <= T-eff <= 100,000 K and 7.0 <= log g <= 9.5. The stellar models are built for pure hydrogen and the spectra cover a wavelength range from 900 angstrom to 2.5 mu m. Additionally, we derive synthetic HST/ACS, HST/WFC3, Bessel UBVRI, and SDSS magnitudes. The grid was also used to model integrated spectral energy distributions of simple stellar populations and our modeling suggests that DAs might be detectable in ultraviolet bands for populations older than similar to 8 Gyr.
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Chen, Eugene Yu-Yu. "White dwarf stars with some hydrogen." Diss., Restricted to subscribing institutions, 2008. http://proquest.umi.com/pqdweb?did=1799891611&sid=6&Fmt=2&clientId=1564&RQT=309&VName=PQD.

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Thompson, A. M. "Energy transport in radially accreting white dwarf stars." Thesis, University of Glasgow, 1986. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.234837.

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Montgomery, Michael Houston. "The evolution and pulsation of crystallizing white dwarf stars /." Full text (PDF) from UMI/Dissertation Abstracts International, 1998. http://wwwlib.umi.com/cr/utexas/fullcit?p9937100.

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Dickinson, Nathan James. "The metal content of hot DA white dwarf spectra." Thesis, University of Leicester, 2012. http://hdl.handle.net/2381/10919.

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In this thesis, a study of the high ionisation-stage metal absorption features in the spectra of hot DA white dwarfs is presented. Metals are present in the photospheres of such stars due to radiative levitation (Chayer et al. 1994, 1995; Chayer Fontaine & Wesemael 1995). However, studies of the patterns between metal abundance and Teff show that, though the broad patterns predicted are seen, individual abundance measurements often do not reflect the predictions of radiative levitation theory (e.g. Barstow et al. 2003b). In this thesis, an analysis of the nitrogen abundance in three stars is performed, where a highly abundant layer of nitrogen was thought to reside at the top of the photospheres of the stars. The nitrogen abundance and distribution in these DAs is found to be homogeneous and of an abundance in keeping with stars of higher Teff. The accretion of metals from circumstellar discs has been shown to be the source of photospheric metals in DAs with Teff < 25,000 K (e.g. Zuckerman et al. 2003), where gravitational diffusion dominates (Koester & Wilken, 2006). In some cases, gaseous components are seen at such discs (e.g. SDSS 122859.93+104032.9; Gänsicke et al. 2006). A survey is made of a sample of hot (19,000 K < Teff < 51,000 K) DAs, where similar accretion may explain the inability of radiative levitation theory alone to account for the detected photospheric metal abundances. No circumstellar gas discs are found, though accretion from as yet undetected circumstellar sources remains an attractive explanation of the photospheric abundances of the stars. Circumstellar absorption is seen in the UV spectra of some hot DA stars (Holberg et al. 1998; Bannister et al. 2003). Sources suggested for this material include circumstellar discs, the ionisation of the ISM, stellar mass loss and planetary nebulae. A re-analysis of this absorption is presented, using a technique that for the first time allows proper modelling of the circumstellar absorption features, and provides column densities for all components. The ionisation of circumstellar discs or planetesimals, the ionisation of the ISM and the ionisation of mass lost by binary companions are put forward as the origin for this circumstellar material.
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Day-Jones, A. C. "Searching for brown dwarf companions." Thesis, University of Hertfordshire, 2009. http://hdl.handle.net/2299/3475.

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In this thesis I present the search for ultracool dwarf companions to main sequence stars, subgiants and white dwarfs. The ultracool dwarfs identified here are benchmark objects, with known ages and distances. The online data archives, the two micron all sky survey (2MASS) and SuperCOSMOS were searched for ultracool companions to white dwarfs, where one M9 1 companion to a DA white dwarf is spectroscopically confirmed as the widest separated system of its kind known to date. The age of the M9 1 is constrained to a minium age of 1.94Gyrs, based on the estimated age of the white dwarf from a spectroscopically derived Teff and log g and an initial-final mass relation. This search was extended using the next generation surveys, the sloan digital sky survey (SDSS) and the UK infrared deep sky survey (UKIDSS), where potential white dwarf + ultracool dwarf binary systems from this search are presented. A handful of these candidate systems were followed-up with second epoch near infrared (NIR) imaging. A new white dwarf with a spectroscopic M4 companion and a possible wide tertiary ultracool component is here confirmed. Also undertaken was a pilot imaging survey in the NIR, to search for ultracool companions to subgiants in the southern hemisphere using the Anglo-Australian telescope. The candidates from that search, as well as the subsequent follow-up of systems through second epoch NIR/optical imaging and methane imaging are presented. No systems are confirmed from the current data but a number of good candidates remain to be followed-up and look encouraging. A search for widely separated ultracool objects selected from 2MASS as companions to Hipparcos main-sequence stars was also undertaken. 16 candidate systems were revealed, five of which had been previously identified and two new L0 2 companions are here confirmed, as companions to the F5V spectroscopic system HD120005 and the M dwarf GD 605. The properties of HD120005C were calculated using the DUSTY and COND models from the Lyon group, and the age of the systems were inferred from the primary members. For GD 605B no age constraint could be placed due to the lack of information available about the primary, but HD120005C has an estimated age of 2-4Gyr. In the final part of this thesis I investigate correlations with NIR broadband colours (J - H, H - K and J - K) with respect to properties, Teff , log g and [Fe/H] for the benchmark ultracool dwarfs, both confirmed from the searches undertaken in this work and those available from the literature. This resulted in an observed correlation with NIR colour and Teff, which is presented here. I find no correlation however with NIR colours and log g or [Fe/H], due in part to a lack of suitable benchmarks. I show that despite the current lack of good benchmark objects, this work has the potential to allow UCD properties to be measured from observable characteristics, and suggest that expanding this study should reveal many more benchmarks where true correlation between properties and observables can be better investigated.
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Snyder, Lucas A. "On the reliability of 2MASS data in identifying red dwarf stars." Virtual Press, 2004. http://liblink.bsu.edu/uhtbin/catkey/1294901.

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Volume-limited samples indicate that red dwarfs are the most abundant stars in the Milky Way and account for most of its mass, despite their low individual masses. However, because of their low luminosity, they are extremely underdetected in magnitude-limited surveys. Complicating the task of identification is the fact that they have the same temperature as red giants and thus are in the same spectral class. We must therefore look for certain spectral features to differentiate between dwarfs and giants. Intermediate-to-broad-band photometry is one method that allows us to perform this task quantitatively. The 2MASS point source catalog contains data for -0.5 billion objects, including photometry in three broadband infrared filters. This paper discusses the manner in which these data can be analyzed to find red dwarfs and the success rate of such analysis.
Department of Physics and Astronomy
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Yeates, Celeste Marie Clemens J. Christopher. "Mode identification from combination frequency amplitudes in pulsating white dwarf stars." Chapel Hill, N.C. : University of North Carolina at Chapel Hill, 2006. http://dc.lib.unc.edu/u?/etd,389.

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Thesis (Ph. D.)--University of North Carolina at Chapel Hill, 2006.
Title from electronic title page (viewed Oct. 10, 2007). "... in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Department of Physics & Astronomy." Discipline: Physics and Astronomy; Department/School: Physics and Astronomy.
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Books on the topic "White dwarf stars Spectra"

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European Workshop on White Dwarfs (7th 1990 Toulouse, France). White dwarfs. Dordrecht: Kluwer Academic, 1991.

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Van Horn, Hugh M. Unlocking the Secrets of White Dwarf Stars. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-09369-7.

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Domitilla, De Martino, ed. White dwarfs. Dordrecht: Kluwer Academic Publishers, 2003.

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European Workshop on White Dwarfs (10th 1996 Blanes, Spain). White dwarfs: Proceedings of the 10th European Workshop on White Dwarfs, held in Blanes, Spain, 17-21 June 1996. Dordrecht: Kluwer Academic Publishers, 1997.

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European, Workshop on White Dwarfs (10th 1996 Blanes Spain). White dwarfs: Proceedings of the 10th Euroepan Workshop on White Dwarfs, held in Blanes, Spain, 17-21 June 1996. Boston, Mass: Kluwer Academic, 1997.

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European Workshop on White Dwarfs (9th 1994 Kiel, Germany). White dwarfs: Proceedings of the 9th European Workshop on White Dwarfs, held at Kiel, Germany, 29 August-1 September 1994. Berlin: Springer, 1995.

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1941-, Koester Detlev, and Moehler S, eds. 14th European Workshop on White Dwarfs: Proceedings of a workshop held in Kiel, Germany, 19-23 July 2004. San Francisco, Calif: Astronomical Society of the Pacific, 2005.

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European Workshop on White Dwarfs (11th 1998 Tromsø, Norway). 11th European Workshop on White Dwarfs: Proceedings of a conference held at Tromsø, Norway, 29 June-3 July, 1998. San Francisco, Calif: Astronomical Society of the Pacific, 1999.

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Ralf, Napiwotzki, and Burleigh Matthew R, eds. 15th European Workshop on White Dwarfs: Proceedings of a meeting held in Leicester, United Kingdom, 7-11 August 2006. San Francisco, Calif: Astronomical Society of the Pacific, 2007.

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Hansen, Carl J. Asteroseismology of white dwarf stars: Final report, 15 Dec 1994-15 Dec 1997 : grant number, NAG 5-2828. [Washington, DC: National Aeronautics and Space Administration, 1998.

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Book chapters on the topic "White dwarf stars Spectra"

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Van Horn, Hugh M. "Decoding the Spectra of White Dwarfs." In Unlocking the Secrets of White Dwarf Stars, 151–63. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-09369-7_14.

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Van Horn, Hugh M. "The Peculiar Spectra of White Dwarfs." In Unlocking the Secrets of White Dwarf Stars, 75–86. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-09369-7_8.

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Van Horn, Hugh M. "The Secrets in the Spectra." In Unlocking the Secrets of White Dwarf Stars, 165–82. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-09369-7_15.

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Väth, H., D. Koester, S. O. Kepler, and E. L. Robinson. "Modeling Time-Resolved Spectra of ZZ Ceti Stars." In White Dwarfs, 481–84. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-011-5542-7_70.

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Aznar Cuadrado, R., and C. S. Jeffery. "Physical Parameters for Subdwarf B Stars with Composite Spectra." In White Dwarfs, 91–92. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0215-8_25.

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Fontaine, G., and F. Wesemael. "Successes and Challenges of the Theory of White Dwarf Spectral Evolution." In Evolution of Stars: The Photospheric Abundance Connection, 421–34. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3416-3_36.

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Bues, I. "Line Band Profiles in the Spectra of Cool Magnetic Helium-Rich White Dwarfs." In Hydrogen Deficient Stars and Related Objects, 391–95. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4744-3_43.

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Bloemen, Steven. "Remarkable Spectral Variability on the Spin Period of the Accreting White Dwarf in V455 And." In High-Precision Studies of Compact Variable Stars, 33–41. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-10283-2_3.

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Lamontagne, R., F. Wesemael, P. Bergeron, J. Liebert, M. S. Fulbright, and R. F. Green. "Feige 55: A Newly—Identified Dao White Dwarf with a Metal—Rich UV Spectrum and a Clue to the Properties of Dao Stars." In White Dwarfs: Advances in Observation and Theory, 347–51. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-2020-3_46.

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Ramspeck, M., U. Heber, S. Moehler, and I. N. Reid. "Spectral Analysis of Supra Horizontal Branch Stars in Globular Clusters." In White Dwarfs, 155–56. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0215-8_44.

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Conference papers on the topic "White dwarf stars Spectra"

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Brassard, P., G. Fontaine, P. Chayer, E. M. Green, Klaus Werner, and T. Rauch. "Computations of NLTE Model Atmospheres and Synthetic Spectra at Université de Montréal: Applications to sdB Stars and AM CVn Systems." In 17TH EUROPEAN WHITE DWARF WORKSHOP. AIP, 2010. http://dx.doi.org/10.1063/1.3527817.

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Ziegler, M., T. Rauch, K. Werner, J. W. Kruk, Klaus Werner, and T. Rauch. "(F)UV Spectral Analysis of Hot, Hydrogen-Rich Central Stars of Planetary Nebulae." In 17TH EUROPEAN WHITE DWARF WORKSHOP. AIP, 2010. http://dx.doi.org/10.1063/1.3527811.

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Adamczak, J., K. Werner, T. Rauch, S. Schuh, J. J. Drake, J. W. Kruk, Klaus Werner, and T. Rauch. "Analysis of Chandra-LETG spectra of two DA white dwarfs and a PG1159 star." In 17TH EUROPEAN WHITE DWARF WORKSHOP. AIP, 2010. http://dx.doi.org/10.1063/1.3527851.

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Kielkopf, J. F., and N. F. Allard. "Lyman series profiles: From laser-plasmas to white dwarf stars." In SPECTRAL LINE SHAPES. ASCE, 1999. http://dx.doi.org/10.1063/1.58340.

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Christova, M., N. F. Allard, J. F. Kielkopf, D. Homeier, F. Allard, Marco Antonio Gigosos, and Manuel Ángel González. "New line profiles of sodium and potassium perturbed by helium for brown dwarf and very cool white dwarf stars." In SPECTRAL LINE SHAPES: Volume 15–19th International Conference on Spectral Line Shapes. AIP, 2008. http://dx.doi.org/10.1063/1.3026467.

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Allard, N. F., I. Drira, and J. F. Kielkopf. "Quasi-molecular satellites in the Lyman β profile: application to the white dwarf stars." In SPECTRAL LINE SHAPES. ASCE, 1999. http://dx.doi.org/10.1063/1.58317.

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Heller, R., D. Homeier, S. Dreizler, R. O̸stensen, and Eric Stempels. "Spectral Analysis of 636 White Dwarf—M Star Binaries from the Sloan Digital Sky Survey." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099271.

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Solheim, J. E., Klaus Werner, and T. Rauch. "Update on AM CVn stars." In 17TH EUROPEAN WHITE DWARF WORKSHOP. AIP, 2010. http://dx.doi.org/10.1063/1.3527826.

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Todt, H., M. Peña, W. R. Hamann, G. Gräfener, Klaus Werner, and T. Rauch. "[WN] central stars of planetary nebulae." In 17TH EUROPEAN WHITE DWARF WORKSHOP. AIP, 2010. http://dx.doi.org/10.1063/1.3527808.

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Castanheira, B. G., S. O. Kepler, S. J. Kleinman, A. Nitta, L. Fraga, Klaus Werner, and T. Rauch. "Discovery of twelve ZZ Ceti stars." In 17TH EUROPEAN WHITE DWARF WORKSHOP. AIP, 2010. http://dx.doi.org/10.1063/1.3527874.

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Reports on the topic "White dwarf stars Spectra"

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Zilberman, Mark. Shouldn’t Doppler 'De-boosting' be accounted for in calculations of intrinsic luminosity of Standard Candles? Intellectual Archive, September 2021. http://dx.doi.org/10.32370/iaj.2569.

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Abstract:
"Doppler boosting / de-boosting" is a well-known relativistic effect that alters the apparent luminosity of approaching/receding radiation sources. "Doppler boosting" alters the apparent luminosity of approaching light sources to appear brighter, while "Doppler de-boosting" alters the apparent luminosity of receding light sources to appear fainter. While "Doppler boosting / de-boosting" has been successfully accounted for and observed in relativistic jets of AGN, double white dwarfs, in search of exoplanets and stars in binary systems it was ignored in the establishment of Standard Candles for cosmological distances. A Standard Candle adjustment appears necessary for "Doppler de-boosting" for high Z, otherwise we would incorrectly assume that Standard Candles appear dimmer, not because of "Doppler de-boosting" but because of the excessive distance, which would affect the entire Standard Candles ladder at cosmological distances. The ratio between apparent (L) and intrinsic (Lo) luminosities as a function of redshift Z and spectral index α is given by the formula ℳ(Z) = L/Lo=(Z+1)^(α-3) and for Type Ia supernova as ℳ(Z) = L/Lo=(Z+1)^(-2). These formulas are obtained within the framework of Special Relativity and may require adjustments within the General Relativity framework.
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