J/A+A/672/A165 Meandering-period Miras (Merchan-Benitez+, 2023)
Meandering periods and asymmetries in light curves of Miras: Observational evidence for low mass-loss rates. Merchan-Benitez P., Uttenthaler S., Jurado-Vargas M. <Astron. Astrophys. 672, A165 (2023)> =2023A&A...672A.165M 2023A&A...672A.165M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Photometry, infrared Keywords: stars: AGB and post-AGB - stars: oscillations - stars: evolution - stars: mass-loss Abstract: Some Miras --- long-period variables in late evolutionary stages --- have meandering pulsation periods and light-curve asymmetries, the causes of which are still unclear. We aim to better understand the origin of meandering periods and light-curve asymmetries by investigating a sample of Miras in the solar neighbourhood. We characterised this group of stars and related their variability characteristics to other stellar parameters. We analysed observations from several databases to obtain light curves with maximum time span and temporal coverage for a sample of 548 Miras. We determined their pulsation-period evolution over a time span of many decades, searched for changes in the periods, and determined the amplitude of the period change. We also analysed the Fourier spectra with respect to possible secondary frequency maxima. The sample was divided into two groups with respect to the presence of light-curve asymmetries (`bumps'). Infrared colours and indicators of the third dredge-up were collected to study the mass loss and deep mixing properties of the stars of our sample. Our analysis reveals one new star, T Lyn, with a continuously changing period. The group of Miras with meandering period changes is exclusively made up of M-type stars. The Fourier spectra of the meandering-period Miras have no prominent additional peaks, suggesting that additional pulsation modes are not the cause of the meandering periods. We confirm that light-curve bumps are more common among S and C Miras and show, for the first time, that Miras with such bumps have lower mass-loss rates than those with regular, symmetric light curves. Also, Miras with meandering period changes have relatively little mass loss. We conclude that Miras with strongly changing periods (including meandering periods) or asymmetries in their light curves have relatively low dust mass-loss rates. Meandering period changes and light-curve asymmetries could be connected to He-shell flashes and third dredge-up episodes. Description: Information is collected for the 548 stars in our sample on the pulsation period (calculated with the VStar 2.21.3 program), the full amplitude of period variations calculated as deltaP/(%), the presence of asymmetry in the light curves (bumps), the technetium content (Tc) and carbon isotope ratios (12C/13C), as well as IR photometry data. Both the name and spectral types are taken from the General Catalog of Variable Stars (GCVS, Samus' et al., 2017, Cat. B/gcvs). The K-band magnitudes were taken from the 2MASS catalogue (Skrutskie et al., 2006, Cat. II/246) or, when available, from the compilation of average magnitudes in Uttenthaler et al. (2019, Cat. J/A+A/622/A120, tablea1). The [3.4] and [22] magnitudes (W1 and W4, respectively) taken from the AllWISE (Cutri et al., 2012, Cat. II/328) or, in case of saturation, from the unWISE catalogue (Schlafly et al., 2019, Cat. II/363). File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tableb1.dat 70 548 Data of pulsation period, deltaP/
, bumps, technetium content, carbon isotope ratios (12C/13C) pulsation properties, and IR photometry of sample stars (corrected version, 07-Apr-2025) -------------------------------------------------------------------------------- See also: B/gcvs : General Catalogue of Variable Stars (Samus+, 2007-2017) II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) II/328 : AllWISE Data Release (Cutri+ 2013) II/363 : The band-merged unWISE Catalog (Schlafly+, 2019) Byte-by-byte Description of file: tableb1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 7 A7 --- GCVS Object name 9- 28 A20 --- SpType Spectral type 30- 34 F5.1 d Period Period calculated with VStar 2.21.3 36- 39 F4.1 % DP/
Full amplitude of period variations, DeltaP/
41 I1 --- Bumps [0/1] Asymmetry in light curves (1) 43- 46 A4 --- Tc Tc content (2) 48 A1 --- r_Tc [a-d] Reference(s) of Tc content (3) 50- 52 I3 --- 12C/13C ? 12C/13C content 54- 56 I3 --- e_12C/13C ? Uncertainty of the 12C/13C content 58 I1 --- r_12C/13C [1/7]? Reference of 12C/13C content (4) 60- 64 F5.3 mag K-[22] Mean K-[22] colour 66- 70 F5.3 mag [3.4]-[22] Mean [3.4]-[22] colour -------------------------------------------------------------------------------- Note (1): Existence of bumps as follows: 0 = Stars with symmetric light curves (Group S) 1 = Stars with asymmetric light curves (Group A) Note (2): Tc content as follows: yes = Yes no = No dbf = Doubtful prob = Probable poss = Possible Note (3): Reference of Tc content as follows: a = Uttenthaler et al., 2019A&A...622A.120U 2019A&A...622A.120U, Cat. J/A+A/622/A120 b = Little et al., 1987AJ.....94..981L 1987AJ.....94..981L c = Uttenthaler et al., in preparation d = Vanture et al., 2007PASP..119..147V 2007PASP..119..147V Note (4): Reference of 12C/13C content as follows: 1 = Hinkle et al., 2016ApJ...825...38H 2016ApJ...825...38H, Cat. J/ApJ/825/38 2 = Ramstedt & Olofsson, 2014A&A...566A.145R 2014A&A...566A.145R 3 = Ohnaka & Tsuji, 1996A&A...310..933O 1996A&A...310..933O, Cat. J/A+A/310/933 4 = Abia & Isern, 1997MNRAS.289L..11A 1997MNRAS.289L..11A 5 = Lebzelter et al., 2019ApJ...886..117L 2019ApJ...886..117L 6 = Schoier & Olofsson, 2000A&A...359..586S 2000A&A...359..586S 7 = Dominy & Wallerstein, 1987ApJ...317..810D 1987ApJ...317..810D -------------------------------------------------------------------------------- Acknowledgements: Stefan Uttenthaler, stefan.uttenthaler(at)gmail.com Pedro Merchan-Benitez, pedromer(at)hotmail.com History: 19-Apr-2023: on-line version 07-Apr-2025: one value corrected
(End) Stefan Uttenthaler [TU Wien], Patricia Vannier [CDS] 01-Mar-2023
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