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LPV News

LPV'S IN THE NEWS

We will include links to recent scientific papers on a regular basis regarding LPV's where AAVSO observations have been used or referenced.

Recent Science Papers (2015-2018)

Mowlavi, M et al "Gaia Data Release 2: The first Gaia catalog of Long Period Variable candidates", May 2018, https://arxiv.org/abs/1805.02035

Kudashkina, L.S; Andronov I.L, "Atlas of the Light Curves and Phase Plane Portraits of Selected Long-Period Variables", November 2017, https://arxiv.org/abs/1711.09029

Kudashkina, L.S; Andronov I.L "Phase Plane Analysis of the Photometrical Variations of Long Period Variables", November 2017, https://arxiv.org/abs/1711.02133

Fucci, A et al "The slowly variable star FY Lacertae", October 2017, https://arxiv.org/abs/1710.07667

Percy, J.R; Laing, J "Amplitude Variations in Pulsating Red Giants. II. Some Systematics", September 2017, https://arxiv.org/abs/1709.09696

Vogt, N et al "Determination of pulsation periods and other parameters of 2875 stars classified as MIRA in the All Sky Automated Survey (ASAS)", The Astrophysical Journal Supplement Series, September 2016, arXiv:1609.05246 [astro-ph.SR]

A.Bodi, et al, "Periodicities of the RV Tau-type pulsating star DF Cygni: a combination of Kepler data with ground-based observations", Astronomy & Astrophysics, September 2016 

Brietenstein, P. et al "Goldilocks Variable - ein Mira-Stern im Hantelnebel M 27", BAV Rundbrief 2/2016, vol. 65, Issue 2, p. 32-39

Uttenthaler, S.; Meingast, S.; Lebzelter, T.; Aringer, B.; Joyce, R. R.; Hinkle, K.; Guzman-Ramirez, L.; Greimel, R., "LX Cygni: A carbon star is born", Astronomy & Astrophysics, Volume 585, A145 (01/2016)

T. Kamiński, K.T. Wong, M. R. Schmidt, H.S.P. Müller, C.A. Gottlieb, I. Cherchneff, K.M. Menten, D. Keller, S. Brünken, J.M. Winters, N.A. Patel, "An observational study of dust nucleation in Mira", Astronomy & Astrophysics April 20, 2016 

K. T. Wong, T. Kamiński, K. M. Menten, F. Wyrowski, "Resolving the extended atmosphere and the inner wind of Mira with long ALMA baselines", Astronomy & Astrophysics March 11, 2016 

M. Wittkowski, A. Chiavassa, B. Freytag, M. Scholz, S. Hoefner, I. Karovicova, P. A. Whitelock, "Near-infrared spectro-interferometry of Mira variables and comparisons to 1D dynamic model atmospheres and 3D convection simulations", Astronomy & Astrophysics 587, A12 (2016)

Chibueze, James; Miyahara, Takeshi; Omodaka, Toshihiro; Ohta,Takashi; Fujii, Takahiro; Tanaka, Masuo; Motohara, Kentaro; Makoto, Miyoshi "Near-infrared Observations of SiO Maser-emitting Asymptotic Giant Branch", (AGB) Stars, The Astrophysical Journal, Volume 817, Issue 2, 115, (2016) 

Wing, Robert F., "Minimum-Light Spectral Classifications for M-Type Mira Variables", IAU General Assembly, Meeting #29, August 2015

Kudashkina, Larisa S.; Andronov, Ivan L.; Marsakova, Vladislava I.; Chinarova, Lidia L., "Statistical Studies of Long - Period Variable Stars in Odessa", Częstochowski Kalendarz Astronomiczny – 2015, ed. Bogdan Wszołek & Agnieszka Kuźmicz  

Keiichi Ohnaka, Gerd Weigelt, Karl-Heinz Hofmann, "Clumpy dust clouds and extended atmosphere of the AGB star W Hya revealed with VLT/SPHERE-ZIMPOL and VLTI/AMBER", Astronomy & Astrophysics, 589, A91 (2016) 

S. Uttenthaler, R. Greimel, M. Templeton, "Is the semi-regular variable RU Vulpeculae undergoing a helium-shell flash?", Astron. Nachr. / AN 999, No. 88, 789 – 795 (2006) 

 

Review Paper on Miras
by Lee Anne Willson and Massimo Morengo
July 18, 2012

Mira variables share essential characteristics: High visual amplitude, periods of hundreds of days, red colors (spectral types M, S, and C), and the presence of emission lines at some phases. They are fundamental mode pulsators, with progenitor masses ranging from >1 to several solar masses. In this review, we summarize what is known from modeling and observational studies, including recent measurements from optical and IR interferometry, and studies involving large samples of stars particularly in the Magellanic Clouds. While we have a good idea of how these stars fit into the big picture of stellar evolution, many important details remain to be settled by a combination of more ambitious models and new observational techniques. Carrying on observations of bright Mira variables will be essential for interpreting observations of large numbers of fainter sources as well as for assessing the completeness and accuracy of the models.

Read the paper on eJAAVSO

 

 

 

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