Relevant bibliographies by topics / Mira variable stars

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  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers

Academic literature on the topic 'Mira variable stars'

Author: Grafiati
Published: 4 June 2021
Last updated: 20 February 2023

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Journal articles on the topic "Mira variable stars"

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Nakagawa, Akiharu, Tomoharu Kurayama, Toshihiro Omodaka, Tatsuya Kamezaki, Yoshiro Nishida, and Makoto Matsui. "The period–luminosity relation of Mira variable stars." Proceedings of the International Astronomical Union 8, S289 (August 2012): 217. http://dx.doi.org/10.1017/s1743921312021412.

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AbstractWe use astrometry to measure the distances to Galactic Mira variable stars. Our purpose is to determine a precise period–luminosity relation (PLR). At present, we do not have a precise PLR for Galactic Mira stars because of the large uncertainties affecting their distance estimates. To reduce the uncertainties, we adopted the Very Long Baseline Interferometry method and measured annual parallaxes of Mira variable stars with VERA. In addition to our previous results, we obtained three new distances for Mira variable stars. Based on our observations, the typical uncertainty in a given distance measurement is reduced to below 10%. At this conference, we present the current status of our project. To establish a precise Galactic PLR, we continue to observe more Mira variables. In addition, the apparent magnitudes of the target stars should be studied carefully.
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Castelaz, Michael W., Donald G. Luttermoser, Daniel B. Caton, and Robert A. Piontek. "Phase-dependent Spectroscopy of Mira Variable Stars." Astronomical Journal 120, no. 5 (November 2000): 2627–37. http://dx.doi.org/10.1086/316837.

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Luttermoser, Donald G., George H. Bowen, and Lee Anne Willson. "NLTE Synthetic Spectra of Mira-Type Variable Stars." International Astronomical Union Colloquium 139 (1993): 207. http://dx.doi.org/10.1017/s025292110011735x.

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AbstractWe present NLTE radiative transfer in hydrodynamic models representative of Mira-type variable stars. Calculations were carried out with the PANDORA code of the Bowen models using a snapshot approximation.
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Iwanek, Patryk, Igor Soszyński, Szymon Kozłowski, Radosław Poleski, Paweł Pietrukowicz, Jan Skowron, Marcin Wrona, et al. "The OGLE Collection of Variable Stars: Nearly 66,000 Mira Stars in the Milky Way." Astrophysical Journal Supplement Series 260, no. 2 (June 1, 2022): 46. http://dx.doi.org/10.3847/1538-4365/ac6676.

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Abstract We present a collection of 65,981 Mira-type variable stars found in the Optical Gravitational Lensing Experiment (OGLE) project database. Two-thirds of our sample (40,356 objects) are located in the Galactic bulge fields, whereas 25,625 stars are in the Galactic disk. The vast majority of the collection (47,532 objects) comprises new discoveries. We provide basic observational parameters of the Mira variables: equatorial coordinates, pulsation periods, I-band and V-band mean magnitudes, I-band brightness amplitudes, and identifications in other catalogs of variable stars. We also provide the I-band and V-band time-series photometry collected since 1997 during the OGLE-II, OGLE-III, and OGLE-IV phases. The classical selection process, i.e., being mostly based on the visual inspection of light curves by experienced astronomers, has led to the high purity of the catalog. As a result, this collection can be used as a training set for machine-learning classification algorithms. Using overlapping areas of adjacent OGLE fields, we estimate the completeness of the catalog to be about 96%. We compare and discuss the statistical features of Miras located in different regions of the Milky Way. We show examples of stars that change their type over time, from a semiregular variable to Mira and vice versa. This data set is perfectly suited to studying the three-dimensional structure of the Milky Way, and it may help to explain the puzzle of the X-shaped bulge.
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Esipov, V. F., M. I. Pashchenko, G. M. Rudnitskij, M. V. Kozin, E. E. Lekht, A. E. Nadjip, and S. V. Fomin. "Multiwavelength Studies of Mira Ceti-type Variable Stars." Symposium - International Astronomical Union 191 (1999): 201–6. http://dx.doi.org/10.1017/s0074180900203082.

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Since 1994, observations of a sample of about 20 Mira Ceti-type and semiregular variables have been carried out in three spectral ranges: radio (H2O maser line λ = 1.35 cm), optical (spectroscopy and UBV photometry) and infrared (JHKLM photometry). Time series of the Hα emission intensity and H2O line flux, covering several periods of the stars, have been obtained. Correlation of the intensity variations of the H2O maser with optical variability in the maser stars RR Aql, U Ori, VX Sgr and others was confirmed. One of the most interesting results is the flare of the H2O maser emission in R Leo, which happened in autumn 1997, 14 months after a flare of the Hα emission.
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Little, S. J., and I. R. Little-Marenin. "The 8-22μm Excess in Carbon Stars From IRAS LRS Spectra." International Astronomical Union Colloquium 106 (1989): 402. http://dx.doi.org/10.1017/s0252921100063429.

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We have measured the excess IR emission from carbon mira and SR variable stars from IRAS LRS spectra. The 8-22μm excess is defined as the ratio of flux above a 2500K energy distribution fit to the LRS spectrum at about 8μm. The carbon star LRS spectra show both emission and absorption features, which are incorporated into our 8-22pm excess. The most prominent feature in carbon stars is the 11.2μm SiC dust emission feature extending from 10μm to 13.8 μm. We observe another emission feature of unknown origin which peaks between 8.4-8.7μm. The SiC emission feature is occasionally blended on the red side by an absorption feature (attributed to gaseous HCN + C2H2) which extends from about 12-16μm. Many of the spectra appear to turn down at the 8μm end due (?) to an HCN + C2H2 absorption feature located at 7.1μm. Carbon stars do not generally show as large an excess as the M mira variables do. The figure below shows our measured excesses for both carbon miras and carbon semi-regular variables. There appears to be little correlation of excess with period, however the mira variables show about twice the range of variation of excess that the semi-regular variables do. We find little correlation between our measured 8-22μm excess and the excesses of Jura (Ap. J., 303, 327, 1986) based on the ratio of 12μm flux to 2μm flux. Our data do support hi s conclusion that longer period variable stars show larger average excesses, but this is only true for mira variables in our analysis.
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Rudnitskij, Georgij M. "Molecular Masers in Variable Stars." Publications of the Astronomical Society of Australia 19, no. 4 (2002): 499–504. http://dx.doi.org/10.1071/as02018.

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AbstractWhen a star with a mass of one to a few solar masses enters the red giant stage of its evolution, the radius of its atmosphere reaches several astronomical units. Pulsational instability is typical for this stage. Most stars become Mira-type or semiregular variables with light cycles of a few hundred days. Red giants lose mass at a rate M = 10−7−10−5M⊙ yr−1. Extensive gas–dust circumstellar envelopes form. These envelopes contain various molecular species. Some of these molecules (OH, H2O, SiO, HCN) manifest themselves in maser radio emission. Data on the H2O maser variability and its connection with the stellar brightness variations are discussed. In the H2O line circumstellar masers can be divided into ‘stable’ (showing persistent emission — R Aql, U Her, S CrB, X Hya) and ‘transient’ (appearing in the H2O line once per 10–15 stellar light cycles — R Leo, R Cas, U Aur). Physical mechanisms of the maser variability are discussed. The most probable process explaining the observed visual–H2O correlation is the influence of shock waves on the masing region. Usually it is assumed that shocks in Mira atmospheres are driven by stellar pulsations. Here an alternative explanation is proposed. If a star during its main sequence life possessed a planetary system, similar to the solar system, the planets will be embedded in a rather dense and hot medium. Effects of a planet revolving around a red giant at a short distance (inside its circumstellar envelope) are discussed. A shock produced by the supersonic motion of a planet can account for the correlated variability of the Hα line emission and H2O maser. If the planetary orbit is highly eccentric, then the connected Hα–H2O flare episodes may be explained by the periastron passage of the planet. New tasks for the upgraded ATCA are discussed.
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Mennessier, Marie-Odile, Hichame Boughaleb, and Janet A. Mattei. "Comparison of Mean Light Curve Parameters of M, S and C Mira and Semi-Regular Variable Stars Using 75 Years of AAVSO Data." Symposium - International Astronomical Union 177 (2000): 165–70. http://dx.doi.org/10.1017/s0074180900002370.

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Using 75 years of AAVSO data, mean light curve parameters of a sample of 350 long-period M, S and C Mira and semi-regular variable stars have been investigated. We compare M, S and C Mira and semi-regular stars, present a classification of the light curves of LPVs and give discriminant parameters.
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Kudashkina, L. S., and I. L. Andronov. "Multiharmonic analysis of Mira-type stars." Symposium - International Astronomical Union 180 (1997): 353. http://dx.doi.org/10.1017/s0074180900131286.

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The shapes of light curves of Mira-type variable stars are analyzed by using the multi–harmonic fit (Andronov 1994). The light curves of 63 stars best covered by the AAVSO observations and published by Mattei (1978) were used. Some correlations between the characteristics of the mean light curves were found.
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Shibahashi, Hiromoto. "Implication of a P-L Relation of Mira Variables." International Astronomical Union Colloquium 139 (1993): 103. http://dx.doi.org/10.1017/s0252921100117014.

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Feast et al. (1989) obtained observationally a period-luminosity (P-L) relation of Mira variables in LMC. Basically, fundamental periods of stellar pulsation should be determined by two quantities —a mass and a radius of the star. The existence of a P-L relation implies a special condition that reduces a function of two variables into a function of only a single variable. Though the AGB appears as a thin line in the HR diagram like the Cepheid instability strip, it is an “asymptotically” merged line of evolutionary tracks of stars in a range of about 0.5-3 solar masses. This fact means that the masses of stars on a point of the AGB are not unique though the radii and the effective temperatures are unique, respectively. Therefore we cannot expect, in the case of AGB stars, that a period is reduced to a function of a single variable.
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Dissertations / Theses on the topic "Mira variable stars"

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Ireland, Michael James. "Optical Interferometry and Mira Variable Stars." University of Sydney. Physics, 2005. http://hdl.handle.net/2123/721.

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This thesis describes the development of a red tip/tilt and fringe detection system at the Sydney University Stellar Interferometer (SUSI), modelling the instrumental performance and effects of seeing at SUSI, making observations of Mira variable stars and finally modelling the atmospheres of Mira variables with physically self-consistent models. The new SUSI tip/tilt system is based around a CCD detector and has been successfully used to both track the majority of tip/tilt power in median seeing at an R magnitude of 4.5, and to provide seeing measures for post processing. The new fringe-detection system rapidly scans 33 to 140 $\mu$m in delay and detects the fringes using two avalanche-photodiodes. It has been used to acquire fringe data, provide user feedback and to track the fringe group-delay position. The system visibility (fringe visibility for a point source) and throughput were found to be consistent with models of the SUSI optical beam train. Observations were made of a variety of sources, including the Mira variables R Car and RR Sco, which were observed in two orthogonal polarization states. These measurements were the first successful use of Optical Interferometric Polarimetry (OIP), and enabled scattered light to be separated from bright photospheric flux. Dust scattering was found to originate from a thin shell 2-3 continuum radii from these stars, with an optical depth of 0.1 to 0.2 at 900 nm. Physical models of Mira variables including dust formation were developed, providing consistent explanations for these results as well as many other photometric and interferometric observations.
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Ireland, Michael. "Optical interferometry and Mira variable stars /." Connect to full text, 2005. http://hdl.handle.net/2123/721.

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Friedman, Vanessa Ann. "Identifying Long Period Variable (LPV) Stars Using Images from the Stardial Observatory." Thesis, The University of Arizona, 2009. http://hdl.handle.net/10150/193423.

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The study of variable stars is extremely important to the astronomical field of scientific research. Variable stars must be methodically studied, usually by amateur astronomers over a long period of time, in order to provide professional astronomers important data that allows them to further analyze variable star behavior.Variable stars are unique because their pulsation produces visible changes in luminosity. This pulsation allows amateur astronomers to visually observe and identify variable stars. This type of research and study is special because amateurs can make a real contribution to the field.My objective was to become an amateur astronomer in the hopes that I could discover variable stars and contribute my findings to the greater astronomical scientific community. In completing this task, my overall goal was to better understand the true nature of science in order to improve my teaching in a secondary science classroom.
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Caddy, Robert V. "Time Series Photometry of the Symbiotic Star V1835 Aql and New Variable Stars in Aquila." Bowling Green State University / OhioLINK, 2018. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1525438143057776.

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Neilson, Hilding, Richard Ignace, Beverly Smith, Gary Henson, and Alyssa Adams. "Evidence of a Mira-like tail and bow shock about the semi-regular variable V CVn from four decades of polarization measurements." Digital Commons @ East Tennessee State University, 2014. https://dc.etsu.edu/etsu-works/6233.

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Polarization is a powerful tool for understanding stellar atmospheres and circumstellar environments. Mira and semi-regular variable stars have been observed for decades and some are known to be polarimetrically variable, however, the semi-regular variable V Canes Venatici displays an unusually large, unexplained amount of polarization. We present ten years of optical polarization observations obtained with the HPOL instrument, supplemented by published observations spanning a total interval of about forty years for V CVn. We find that V CVn shows large polarization variations ranging from 1 - 6%. We also find that for the past forty years the position angle measured for V CVn has been virtually constant suggesting a long-term, stable, asymmetric structure about the star. We suggest that this asymmetry is caused by the presence of a stellar wind bow shock and tail, consistent with the star's large space velocity.
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Cardona, Velasquez Gustavo Adolfo. "Properties of Bright Variable Stars in Unusual Metal Rich Cluster NGC 6388." Bowling Green State University / OhioLINK, 2011. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1308577583.

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Kager, Elisabeth. "Pulsation Properties of Long Period Variable Stars in Globular Cluster NGC 6553." Bowling Green State University / OhioLINK, 2010. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1277148078.

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Aljassim, Mohammad A. "A 6-Year Study of Long Period Variable Stars in the Globular Cluster NGC 6388." Bowling Green State University / OhioLINK, 2017. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1499442952467274.

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Abbas, Mohamad. "A search for Long-Period Variable Stars in the Globular Cluster NGC 6496." Bowling Green State University / OhioLINK, 2011. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1308597257.

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Tuthill, Peter George. "Imaging stars through the atmosphere." Thesis, University of Cambridge, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.337414.

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Books on the topic "Mira variable stars"

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United States. National Aeronautics and Space Administration., ed. Final report to the National Aeronautics and Space Administration concerning the Astrophysical Data Program entitled, The chromosphere/shock dilemma of non-Mira, late-type variable stars: NASA grant number NAG 5-2830 : report covering the period, 12/15/94-12/14/96. [Washington, DC: National Aeronautics and Space Administration, 1997.

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United States. National Aeronautics and Space Administration., ed. Final report to the National Aeronautics and Space Administration concerning the Astrophysical Data Program entitled, The chromosphere/shock dilemma of non-Mira, late-type variable stars: NASA grant number NAG 5-2830 : report covering the period, 12/15/94-12/14/96. [Washington, DC: National Aeronautics and Space Administration, 1997.

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Book chapters on the topic "Mira variable stars"

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Yi, Jiyune, R. S. Booth, and J. E. Conway. "Phase Dependence of 43 GHz SiO Masers in the Mira Variable TX Cam." In Mass-Losing Pulsating Stars and their Circumstellar Matter, 295–98. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0139-7_68.

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Sato, Koichi, Masanori Yoshizawa, Jun Nishikawa, Naoko Ohishi, and Takayuki Kotani. "Mira Project and the Observations of Mira Variables." In Mass-Losing Pulsating Stars and their Circumstellar Matter, 405–8. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0139-7_91.

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Zijlstra, Albert A., Mikako Matsuura, and Timothy R. Bedding. "Period Evolution in Mira Variables." In Mass-Losing Pulsating Stars and their Circumstellar Matter, 91–94. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0139-7_13.

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Groenewegen, M. A. T., P. A. Whitelock, C. H. Smith, and F. Kerschbaum. "Dust Shells around Carbon Mira Variables." In Dust and Molecules in Evolved Stars, 89–96. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-017-1307-8_11.

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Vardya, M. S. "Some Properties of S Mira Variables." In Cool Stars with Excesses of Heavy Elements, 105–9. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5325-3_14.

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Feast, Michael. "The Galactic Kinematics of Mira Variables." In Mass-Losing Pulsating Stars and their Circumstellar Matter, 83–89. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0139-7_12.

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Hinkle, Kenneth H., and Werner W. G. Scharlach. "Carbon Isotope Ratios in Oxygen Rich Mira and SRa Variables." In Cool Stars with Excesses of Heavy Elements, 255–59. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5325-3_33.

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Humphreys, E. M. L., M. D. Gray, D. Field, J. A. Yates, and G. Bowen. "A Model for the Variability of SiO Masers in Mira Variables." In Dust and Molecules in Evolved Stars, 215–18. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-017-1307-8_31.

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Onaka, Takashi, Teije de Jong, and Issei Yamamura. "Time Variation of Mid-Infrared Spectra of M-Type Mira Variables." In Mass-Losing Pulsating Stars and their Circumstellar Matter, 257–58. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0139-7_62.

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Kurayama, Tomoharu, and Tetsuo Sasao. "Annual Parallax Measurements of Mira-Type Variables with Phase-Reference VLBI Observation." In Mass-Losing Pulsating Stars and their Circumstellar Matter, 233–34. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0139-7_50.

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Conference papers on the topic "Mira variable stars"

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Karovicova, Iva, Markus Wittkowski, David A. Boboltz, Michael Scholz, and Eric Stempels. "Coordinated AMBER and MIDI observations of the Mira variable RR Aql." 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/10.1063/1.3099285.

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