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Journal articles on the topic 'Variable stars'

Author: Grafiati

Published: 4 June 2021

Last updated: 25 July 2025

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1

Szeidl, B., M. Breger, A. N. Cox, et al. "27. Variable Stars (Etoiles Variables)." Transactions of the International Astronomical Union 20, no. 1 (1988): 257–92. http://dx.doi.org/10.1017/s0251107x00007197.

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The field of variable star research has become so broad and the amount of research to be reported on has grown so rapidly that it is a vain hope that a report of this kind, in a very limited space, could cover the whole field of research and could mention all the papers that have been published in the last three years. It is only hoped that this report presents the significant results achieved in the field of the most important aspects of variable star research. Some important subjects (e.g. cataclysmic variables) relevant to the variable star research are reviewed in the reports of other comm

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2

Percy, J. R., L. Szabados, K. Oláh, et al. "27. Variable Stars (Etoiles Variables)." Transactions of the International Astronomical Union 22, no. 1 (1994): 243–76. http://dx.doi.org/10.1017/s0251107x00008051.

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3

Jerzykiewicz, M., L. A. Baiona, E. F. Guinan, et al. "Division V: Variable Stars: (Etoiles Variables)." Transactions of the International Astronomical Union 24, no. 1 (2000): 251–54. http://dx.doi.org/10.1017/s0251107x0000314x.

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This report covers the period July 1, 1996 (the closing date of the reports in the IAU Trans. 23A) through August 31, 1999. Since the reports of Commissions 27 and 42 that follow highlight the research made in the triennium, we limit ourselves here to organizational activities of the Division. The first three sections are devoted to the General Catalogue of Variable Stars (GCVS), the Information Bulletin on Variable Stars (IBVS), and the Archives of Unpublished Observations of Variable Stars, the important projects that serve us all. I am indebted to the authors, listed in the sections heading

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4

Guinan, Edward F., S. Balona, J. Christensen-Dalgaard, et al. "Division V: Variable Stars: (Etoiles Variables)." Transactions of the International Astronomical Union 25, no. 1 (2002): 265–67. http://dx.doi.org/10.1017/s0251107x00001528.

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Christensen-Dalsgaard, Jørgen, Conny Aerts, Carla Cacciari, et al. "Commission 27: Variable Stars: (Etoiles Variables)." Transactions of the International Astronomical Union 25, no. 1 (2002): 271–76. http://dx.doi.org/10.1017/s0251107x00001553.

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6

Percyy, John R. "Variable stars." Physics Teacher 31, no. 9 (1993): 541–43. http://dx.doi.org/10.1119/1.2343874.

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7

Kurtz, D. W., J. Christensen-Dalsgaard, C. Cacciari, et al. "Commission 27: Variable Stars: (Les Etoiles Variables)." Transactions of the International Astronomical Union 24, no. 1 (2000): 255–58. http://dx.doi.org/10.1017/s0251107x00003151.

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For Commission 27 these triennial reports have traditionally been very compact literature reviews of all the fields relevant to our commission. For several triennia we have been discussing the relevance of them, and asking just who their readership is. It seems that only a few people read them, and fewer use them as introductions to the subject – supposedly one of their prime purposes. The major beneficiaries have been the writers, who have been forced to do three-year reviews of their subjects. The IAU EC gave us the option this triennium of a shorter, four-page report to which the majority o

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8

Christensen-Dalsgaard, Jørgen. "Commission 27: Variable Stars (Les Étoiles Variables)." Transactions of the International Astronomical Union 25, no. 2 (2007): 149–50. http://dx.doi.org/10.1017/s0251107x00026705.

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9

Warner, Brian. "Cataclysmic Variable Stars." Highlights of Astronomy 11, no. 1 (1998): 16–27. http://dx.doi.org/10.1017/s1539299600019924.

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The evolution of single stars on and away from the main sequence is well understood. A degenerate core is formed in a star as the star leaves the main sequence and expands to a giant with a radius typically 50 - 500 Ro . Observationally it is known that most stars are members of binary systems, and among these many have orbital periods less than 100 y. It can happen, therefore, that the expanding envelope of the primary of a binary system can reach to the secondary. As this happens, the primary fills its Roche tidal lobe and transfers matter to the secondary; if the primary has a radiative env

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10

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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11

Warner, Brian, and Scott Kenyon. "Cataclysmic Variable Stars." Physics Today 49, no. 11 (1996): 88–89. http://dx.doi.org/10.1063/1.881529.

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12

Kudashkina, L. S. "Semiregular Variable Stars." Astrophysics 62, no. 4 (2019): 556–72. http://dx.doi.org/10.1007/s10511-019-09604-4.

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13

Burnashev, V. I., and B. A. Burnasheva. "Edward Schoenfeld: Visual photometry of variable stars. 2. Variable stars." Bulletin of the Crimean Astrophysical Observatory 105, no. 1 (2009): 78–81. http://dx.doi.org/10.3103/s0190271709010100.

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14

Zhou, Ai-Ying. "Identifying SuperWASP Detected Candidate Variables with TESS*." Research Notes of the AAS 7, no. 10 (2023): 227. http://dx.doi.org/10.3847/2515-5172/ad06b9.

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Abstract Using Transiting Exoplanet Survey Satellite light curves, I have identified more than 1200 new pulsating variable stars from the SuperWASP-detected but unclassified candidate variables. These include a variety of types of pulsating variable stars, including 125 δ Scuti stars, 235 γ Doradus stars, 302 RR Lyrae stars, and 450+ Mira/SR/IR/LPV variables. I also identified 1300+ rotating variable stars. Additionally, I revealed that 16 of 91 newly identified eclipsing binary systems have pulsating components. These findings will help us to better understand the properties and evolution of

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Gao, Xinyi, Xiaodian Chen, Shu Wang, and Jifeng Liu. "Classification of Periodic Variable Stars from TESS." Astrophysical Journal Supplement Series 276, no. 2 (2025): 57. https://doi.org/10.3847/1538-4365/ad9dd6.

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Abstract The number of known periodic variable stars has increased rapidly in recent years. As an all-sky transit survey, the Transiting Exoplanet Survey Satellite (TESS) plays an important role in detecting low-amplitude variable stars. Using 2 minute cadence data from the first 67 sectors of TESS, we find 72,505 periodic variable stars. We used 19 parameters including period, physical parameters, and light-curve (LC) parameters to classify periodic variable stars into 12 subtypes using the random forest method. Pulsating variable stars and eclipsing binaries are distinguished mainly by perio

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Michalska, Gabriela. "Variable stars in young open cluster NGC 2244." Monthly Notices of the Royal Astronomical Society 487, no. 3 (2019): 3505–22. http://dx.doi.org/10.1093/mnras/stz1500.

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ABSTRACT We present results of a UBVIC variability survey in the young open cluster NGC 2244. In total, we found 245 variable stars. Most of them, 211 stars, are variables with irregular variations. Furthermore, 23 periodic variables were found. We also detected four candidates for δ Scuti stars and seven eclipsing binaries. Based on the mid-infrared Spitzer and WISE photometry and near infrared JHKS 2MASS photometry, we classified 104 young stellar sources among our variables: 1 Class I object, 1 Class I/flat spectrum object, 4 flat spectrum objects, 91 Class II objects, and 7 transition disc

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17

Morris, S. L. "The ellipsoidal variable stars." Astrophysical Journal 295 (August 1985): 143. http://dx.doi.org/10.1086/163359.

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18

Christensen-Dalsgaard, Jørgen, Alvaro Giménez, Edward F. Guinan, Conny Aerts, Luis A. Balona, and Jorge Sahade. "DIVISION V: VARIABLE STARS." Proceedings of the International Astronomical Union 3, T26B (2007): 165–67. http://dx.doi.org/10.1017/s1743921308023946.

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Division V provides a joint forum for the study of stellar variability in all its manifestations, whether due to pulsation, surface inhomogeneities, evolutionary changes, or to eclipses and other phenomena specifically related to double and multiple stars.

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Aerts, Conny, Steven D. Kawaler, Jørgen Christensen-Dalsgaard, et al. "COMMISSION 27: VARIABLE STARS." Proceedings of the International Astronomical Union 3, T26B (2007): 168–70. http://dx.doi.org/10.1017/s1743921308023958.

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The meeting started at 16h00. The president welcomed the 24 participants to the business meeting of Commission 27. After the approval of the agenda, she gave an overview of the activities of Commission 27 of the past three years.

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Giménez, Alvaro, Steven D. Kawaler, Conny Aerts, et al. "DIVISION V: VARIABLE STARS." Proceedings of the International Astronomical Union 4, T27A (2008): 251–53. http://dx.doi.org/10.1017/s1743921308025623.

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Division V deals with all aspects of stellar variability, either intrinsic or due to eclipses by its companion in a binary system. In the case of intrinsic stellar variability the analysis of pulsating stars, surface inhomogeneities, stellar activity and oscillations are considered. For close binaries, classical detached eclipsing binaries are studied as well as more interacting systems, like contact and semi-detached binaries, or those with compact components, like cataclysmic variables and X-ray binaries, including the physics of accretion processes.

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Kawaler, Steven D., Gerald Handler, Conny Aerts, et al. "COMMISSION 27: VARIABLE STARS." Proceedings of the International Astronomical Union 4, T27A (2008): 254–59. http://dx.doi.org/10.1017/s1743921308025635.

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The Organizing Committee of Commission 27 has decided to again provide a somewhat abbreviated bibliography as part of this triennial report, as astronomy-centered search engines and on-line publications continue to blossom. We focus on selected highlights in variable star research over the past three years. Further results can be found in numerous proceedings of conferences held in the time frame covered by this report.

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22

Christensen-Dalsgaard, Jørgen, Conny Aerts, Alvaro Giménez, Edward F. Guinan, Luis A. Balona, and Jorge Sahade. "Division V: Variable Stars." Proceedings of the International Astronomical Union 1, T26A (2005): 245. http://dx.doi.org/10.1017/s1743921306004637.

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Division V, “Variable Stars”, consists of Commission 27, also called “Variable Stars” and Commission 42, “Close Binaries”. Thus the former deals with stars whose variations are intrinsic, whereas in the latter the variations are caused by the interactions between the components in the binary. It is evident that the definition of the Division is predominantly observational, and there may be cases where the assignment of an object to one of the two commissions might be in doubt (a recent somewhat related example was the first detection of an extra-solar planet, in 54 Pegasi, where intrinsic vari

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23

Aerts, Conny, Steven Kawaler, Tim Bedding, et al. "Commission C27: Variable Stars†." Proceedings of the International Astronomical Union 1, T26A (2005): 247–58. http://dx.doi.org/10.1017/s1743921306004649.

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AbstractWe report the major highlights of variable star research within the past three years. This overview is limited to intrinsically variable stars, because the achievements in variable star research stemming from binarity, or multiplicity in general, is covered by the summary report of Commissions 26 and 42.

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24

Gimenez, Alvaro, Steven Kawaler, Jørgen Christensen-Dalsgaard, Michel Breger, Edward Guinan, and Slavek Rucinski. "DIVISION V: VARIABLE STARS." Proceedings of the International Astronomical Union 6, T27B (2010): 207–8. http://dx.doi.org/10.1017/s1743921310005107.

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Division V organized a brief Business meeting during the XXVIIth General Assembly, prior to Business meetings (reported separately) of Commissions 27 and 42. The Division V Business Meeting began at 11:00 on 5 August 2009.

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Kawaler, Steven D., Gerald Handler, Conny Aerts, et al. "COMMISSION 27: VARIABLE STARS." Proceedings of the International Astronomical Union 6, T27B (2010): 209–10. http://dx.doi.org/10.1017/s1743921310005119.

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The meeting started at 14h00. The president welcomed the participants to the business meeting of C27, and acknowledged the members of the Organizing Committee. Special thanks were expressed to the outgoing members: Conny Aerts, Peter Martinez, and Seetha Somasundaram.

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26

Kawaler, Steven D., Ignasi Ribas, Alvaro Gimenez, et al. "DIVISION V: VARIABLE STARS." Proceedings of the International Astronomical Union 7, T28A (2011): 211–12. http://dx.doi.org/10.1017/s1743921312002839.

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27

Handler, Gerald, Karen R. Pollard, Steven Kawaler, et al. "COMMISSION 27: VARIABLE STARS." Proceedings of the International Astronomical Union 7, T28A (2011): 213–18. http://dx.doi.org/10.1017/s1743921312002840.

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28

Eyer, Laurent, Berry Holl, and Nami Mowlavi. "Gaia and variable stars." Proceedings of the International Astronomical Union 9, S298 (2013): 265–68. http://dx.doi.org/10.1017/s1743921313006455.

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AbstractThe study of variable phenomena (periodic, irregular or transient) provides a unique way to acquire knowledge about objects in our Universe. Currently, we are going through a rapid expansion of time-domain astrophysics. One reason for this expansion is the technological developments materialised in small to medium size observational projects such as HAT, OGLE, Catalina, PTF and upcoming very large projects such as Gaia or LSST.In this article, we are focusing on the ESA cornerstone mission Gaia. This spacecraft will provide astrometric, photometric and spectroscopic measurements for on

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Ahmad Dar, Ajaz, Padmakar Singh Parihar, Parvej Saleh, and Manzoor Ahmad Malik. "Variable stars in M37." Research in Astronomy and Astrophysics 18, no. 12 (2018): 155. http://dx.doi.org/10.1088/1674-4527/18/12/155.

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30

Kazarian, M. A., and G. V. Petrosian. "Three New Variable Stars." Astrophysics 46, no. 4 (2003): 502–5. http://dx.doi.org/10.1023/b:asys.0000003266.19893.37.

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31

Maurya, Jayanand, Y. C. Joshi, A. Panchal, and A. S. Gour. "Investigating Stellar Variability in the Open Cluster Region NGC 381." Astronomical Journal 165, no. 3 (2023): 90. http://dx.doi.org/10.3847/1538-3881/acad7e.

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Abstract We study variable stars in the field of the open cluster NGC 381 using photometric data observed over 27 nights and identify a total of 57 variable stars, six of which are member stars. The variable stars are classified based on their periods, amplitudes, light-curve shapes, and locations in the H-R diagram. We found a rich variety of variable stars in the cluster. We identified a total of 10 eclipsing binaries, of which two are of Algol type while eight are of W UMa type (EW). The estimated ages of these EW binaries are greater than 0.6 Gyr, which is in agreement with the formation t

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Wang, Hong, Yu Zhang, Xiangyun Zeng, et al. "Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region." Astronomical Journal 164, no. 2 (2022): 40. http://dx.doi.org/10.3847/1538-3881/ac755a.

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Abstract We have investigated the variable stars in the field surrounding NGC 2355 based on the time-series photometric observation data. More than 3000 CCD frames were obtained in the V band spread over 13 nights with the Nanshan One-meter Wide-field Telescope. We have detected 88 variable stars, containing 72 new variable stars and 16 known variable stars. By analyzing these light curves, we classified the variable stars as follows: 26 eclipsing binaries, 52 pulsating stars, four rotating variables, and six unclear type-variable stars for which their periods are much longer than the time bas

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Goldsmith, C. G. "Variable Stars in the Sculptor Dwarf Galaxy." International Astronomical Union Colloquium 139 (1993): 358. http://dx.doi.org/10.1017/s025292110011783x.

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This project was initiated in 1985 by James Nemec (University of Washington) and Nicholas Suntzeff (C.T.I.O.). The goal was to study the system of ∼600 variable stars in the Sculptor dwarf galaxy. In 1987 the author became the recipient of the plate collection, which formed the basis for his Ph.D. dissertation. In this paper preliminary results are presented. Briefly, 612 stars were studied, of which 432 are van Agt (1978) stars and 180 are newly discovered variable stars. A total of 381 stars are confirmed variables. Most of these are RR Lyraes, but many anomalous Cepheids and some candidate

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Bernhard, Klaus, Stefan Hümmerich, Ernst Paunzen, and Johana Supíková. "New magnetic chemically peculiar stars and candidates in the ATLAS first catalogue of variable stars." Monthly Notices of the Royal Astronomical Society 506, no. 3 (2021): 4561–77. http://dx.doi.org/10.1093/mnras/stab2065.

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ABSTRACT The number of known variable stars has increased by several magnitudes over the last decade, and automated classification routines are becoming increasingly important to cope with this development. Here we show that the ‘upside-down CBH variables’, which were proposed as a potentially new class of variable stars by Heinze et al. in the ATLAS First Catalogue of Variable Stars, are, at least to a high percentage, made up of α2 Canum Venaticorum (ACV) variables – that is, photometrically variable magnetic chemically peculiar (CP2/He-peculiar) stars – with distinct double-wave light curve

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35

Samus, Nikolay N., Elena V. Kazarovets, and Olga V. Durlevich. "Catalogs of variable stars, current and future." Proceedings of the International Astronomical Union 5, S264 (2009): 496–98. http://dx.doi.org/10.1017/s174392130999319x.

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AbstractTo study effects of stellar variability, it is necessary to have complete lists of variable stars with good coordinates, correct variability ranges, reliable classification. The General Catalogue of Variable Stars (GCVS) is one of the main sources of information of this kind. Recently, the flow of information on stellar variability has increased strongly, requiring new approaches to GCVS compilation. New classification schemes are needed for variable stars, taking into account the development of our knowledge. We present information on the current state of the GCVS, its web data base,

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Shipman, H. L. "Variable white dwarfs." Proceedings of the International Astronomical Union 15, S357 (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 th

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Smith, Richard, Avi Patel, Monika D. Soraisam, et al. "Variable Stars in M31 Stellar Clusters from the Panchromatic Hubble Andromeda Treasury." Astrophysical Journal 974, no. 2 (2024): 292. http://dx.doi.org/10.3847/1538-4357/ad6eff.

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Abstract Variable stars in stellar clusters can offer key constraints on stellar evolution and pulsation models, utilizing estimates of host cluster properties to constrain stellar physical parameters. We present a catalog of 86 luminous (F814W < 19) variable stars in M31 clusters identified by mining the archival Panchromatic Hubble Andromeda Treasury (PHAT) survey using a combination of statistical analysis of sparse PHAT light curves and difference imaging. We determine the evolutionary phases and initial masses of these variable stars by matching them with theoretical isochrones generat

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Chen, Xiaodian, Shu Wang, Licai Deng, et al. "China Space Station Telescope and Variable Star Studies." Proceedings of the International Astronomical Union 18, S376 (2022): 319–27. http://dx.doi.org/10.1017/s1743921323003101.

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AbstractIn the last five years, the number of periodic variable stars has increased by two million. We used the ZTF DR2 data to find and build a catalog that includes 780,000 periodic variable stars. These periodic variable stars were classified into 11 types, which greatly complemented the variable stars in Galactic disk. Based on the latest ZTF DR16 data, we found 2 million variable candidates. We trained a machine learner to classify variable stars, and the learner had a prediction accuracy of 94%. Using millions of variable stars, we carried out studies to optimize the period–luminosity re

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Sowicka, P., G. Handler, R. Taubner, et al. "Variable stars in the field of the young open cluster Roslund 2." Proceedings of the International Astronomical Union 9, S301 (2013): 495–96. http://dx.doi.org/10.1017/s1743921313015226.

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AbstractThe study of variable stars in open clusters via asteroseismology is a powerful tool for the study of stellar evolution and stars in general. That is because stars in clusters can be assumed to originate from the same interstellar cloud, so they share similar properties such as age and overall metallicity. We performed a search for variable stars in the field of the young open star cluster Roslund 2, with photoelectric and CCD photometry acquired at two different telescopes. Within the resulting light curves we have found 12 variable stars. Our measurements confirm three previously kno

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Sinha, Tirthendu, Saurabh Sharma, A. K. Pandey, et al. "Variable stars in the Sh 2-170 H ii region." Monthly Notices of the Royal Astronomical Society 493, no. 1 (2020): 267–87. http://dx.doi.org/10.1093/mnras/staa206.

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ABSTRACT We present multi-epoch deep (∼20 mag) Ic-band photometric monitoring of the Sh 2-170 star-forming region to understand the variability properties of pre-main-sequence (PMS) stars. We report identification of 47 periodic and 24 non-periodic variable stars with periods and amplitudes ranging from ∼4 h to 18 d and from ∼0.1 to 2.0 mag, respectively. We have further classified 49 variables as PMS stars (17 Class ii and 32 Class iii) and 17 as main-sequence (MS)/field star variables. A larger fraction of MS/field variables (88 per cent) show periodic variability as compared to the PMS vari

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Burggraaff, O., G. J. J. Talens, J. Spronck, et al. "Studying bright variable stars with the Multi-site All-Sky CAmeRA (MASCARA)." Astronomy & Astrophysics 617 (September 2018): A32. http://dx.doi.org/10.1051/0004-6361/201833142.

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Context. The Multi-site All-Sky CAmeRA (MASCARA) aims to find the brightest transiting planet systems by monitoring the full sky at magnitudes 4 < V < 8.4, taking data every 6.4 s. The northern station has been operational on La Palma since February 2015. These data can also be used for other scientific purposes, such as the study of variable stars. Aims. In this paper we aim to assess the value of MASCARA data for studying variable stars by determining to what extent known variable stars can be recovered and characterised, and how well new, unknown variables can be discovered. Methods.

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Aathil, Abdullah Mohamed. "Review on Photometric Study of Variable Stars." Acceleron Aerospace Journal 2, no. 6 (2024): 316–28. http://dx.doi.org/10.61359/11.2106-2425.

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This literature review focuses on variable stars, which exhibit changes in brightness over time. This topic is vital in astronomical research, particularly due to the abundance of telescope data available in archives. The photometric study of variable stars is significant for understanding stellar evolution, classifying stars, and contributing to cosmological research. It enables precise distance measurements, examines exoplanetary systems, and identifies rare astronomical phenomena, thereby expanding our understanding of the universe. The study begins by outlining the fundamentals of variable

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43

Handler, G. "Variable central stars of young Planetary Nebulae." Symposium - International Astronomical Union 180 (1997): 109. http://dx.doi.org/10.1017/s0074180900129973.

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Three different kinds of variable stars can be found among central stars of Planetary Nebulae. Close binary central stars change their light level because of eclipses and due to the reflection effect; some hot variables have been identified as multiperiodic pulsators (e.g. see Ciardullo & Bond 1996).

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Chan, Ho-Sang, V. Ashley Villar, Siu-Hei Cheung, et al. "Searching for Anomalies in the ZTF Catalog of Periodic Variable Stars." Astrophysical Journal 932, no. 2 (2022): 118. http://dx.doi.org/10.3847/1538-4357/ac69d4.

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Abstract Periodic variables illuminate the physical processes of stars throughout their lifetime. Wide-field surveys continue to increase our discovery rates of periodic variable stars. Automated approaches are essential to identify interesting periodic variable stars for multiwavelength and spectroscopic follow-up. Here we present a novel unsupervised machine-learning approach to hunt for anomalous periodic variables using phase-folded light curves presented in the Zwicky Transient Facility Catalogue of Periodic Variable Stars by Chen et al. We use a convolutional variational autoencoder to l

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Feast, Michael, and Patricia A. Whitelock. "Variable Stars and Galactic Structure." Proceedings of the International Astronomical Union 9, S298 (2013): 40–52. http://dx.doi.org/10.1017/s1743921313006182.

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AbstractVariable stars have a unique part to play in Galactic astronomy. Among the most important of these variables are the Cepheids (types I and II), the RR Lyraes and the Miras (O- and C-rich). The current status of the basic calibration of these stars in their roles as distance, structure and population indicators is outlined and some examples of recent applications of these stars to Galactic and extragalactic problems are reviewed. The expected impact of Gaia on this type of work is discussed and the need for complementary ground based observations, particularly large scale near-infrared

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Paunzen, E., M. Zejda, Z. Mikulášek, et al. "Variable stars in open clusters." Proceedings of the International Astronomical Union 9, S301 (2013): 471–72. http://dx.doi.org/10.1017/s174392131301510x.

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AbstractWe present our joint efforts to study variable stars in open clusters. This includes a new catalogue, a photometric survey for new variables, and the database WEBDA. Our tools will shed more light on stellar variability in open clusters.

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Dougherty, S. M., and A. R. Taylor. "Identifying near-IR variable Be stars." Symposium - International Astronomical Union 162 (1994): 416–17. http://dx.doi.org/10.1017/s0074180900215520.

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Near-IR variable Be stars are identified from multi-epoch observations spanning 20 years using a statistical technique. In this manner, observations from different observing sites can be meaningfully combined and compared. A more thorough investigation of the incidence and properties of IR variability in Be stars as a class of stars is then possible.

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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

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Ruban, E. V., G. A. Alekseeva, A. A. Arkharov, et al. "Spectrophotometric observations of variable stars." Astronomy Letters 32, no. 9 (2006): 604–7. http://dx.doi.org/10.1134/s1063773706090052.

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Valenzuela, Lucas, and Karim Pichara. "Unsupervised classification of variable stars." Monthly Notices of the Royal Astronomical Society 474, no. 3 (2017): 3259–72. http://dx.doi.org/10.1093/mnras/stx2913.

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