RR-Lyrae-type pulsations from a 0.26-solar-mass star in a binary system

Pietrzyński, G.; Thompson, I. B.; Gieren, W.; Graczyk, D.; Stępień, K.; Bono, G.; Moroni, P. G. Prada; Pilecki, B.; Udalski, A.; Soszyński, I.; Preston, George W.; Nardetto, N.; McWilliam, A.; Roederer, Ian U.; Górski, Marek; Konorski, P.; Storm, J.

doi:10.1038/nature10966

Cited by 111 publications

(119 citation statements)

References 14 publications

(14 reference statements)

Supporting

Mentioning

112

Contrasting

Unclassified

Order By: Relevance

“…Let us mention the discovery of a new class of double-mode RR Lyr variables (anomalous RRd stars, [56]), the detection of non-radial modes in RR Lyr stars (e.g., [22]), the first observations of the Blazhko effect in RRd stars ( [38]), RR Lyr stars switching their pulsation modes ( [50,51]), and a candidate for an RR Lyr star in an eclipsing binary system (OGLE-BLG-RRLYR-02792), which turned out to be the first known representative of a new type of pulsating stars mimicking classical RR Lyr stars ( [32]). …”

Section: Rr Lyrae Starsmentioning

confidence: 99%

The impact of large-scale, long-term optical surveys on pulsating star research

Soszyński

2017

EPJ Web Conf.

View full text Add to dashboard Cite

Abstract. The era of large-scale photometric variability surveys began a quarter of a century ago, when three microlensing projects -EROS, MACHO, and OGLE -started their operation. These surveys initiated a revolution in the field of variable stars and in the next years they inspired many new observational projects. Large-scale optical surveys multiplied the number of variable stars known in the Universe. The huge, homogeneous and complete catalogs of pulsating stars, such as Cepheids, RR Lyrae stars, or long-period variables, offer an unprecedented opportunity to calibrate and test the accuracy of various distance indicators, to trace the three-dimensional structure of the Milky Way and other galaxies, to discover exotic types of intrinsically variable stars, or to study previously unknown features and behaviors of pulsators. We present historical and recent findings on various types of pulsating stars obtained from the optical large-scale surveys, with particular emphasis on the OGLE project which currently offers the largest photometric database among surveys for stellar variability.

show abstract

Section: Rr Lyrae Starsmentioning

confidence: 99%

The impact of large-scale, long-term optical surveys on pulsating star research

Soszyński

2017

EPJ Web Conf.

View full text Add to dashboard Cite

show abstract

“…Our plotted values are the solar metallicity ones. [17] found an RR Lyrae with 0.26 M , and [16] found a 0.23 M pulsating subdwarf (sdBV). Interacting binary with mass exchange models by [13] show that during a hydrogen shell burning pulse, an extremely low mass white dwarf can cross the main sequence, horizontal branch and even giant instability strip.…”

Section: Introductionmentioning

confidence: 98%

Pulsating white dwarfs

Romero

2017

EPJ Web Conf.

View full text Add to dashboard Cite

Abstract. The Sloan Digital Sky Survey has allowed us to increase the number of known white dwarfs by a factor of five and consequently the number of known pulsating white dwarfs also by a factor of five. It has also led to the discovery of new types of variable white dwarfs, as the variable hot DQs, and the pulsating Extremely Low Mass white dwarfs. With the Kepler Mission, it has been possible to discover new phenomena, the outbursts present in a few pulsating white dwarfs.

show abstract

“…Other physical characteristics also indicate that this binary component is a very special object as a result of an evolution in a close binary followed by a life similar to a classical RR Lyrae star. Pietrzyński et al (2012) included the object in a new class of pulsating stars called binary evolution pulsators (BEP). OGLE-LMC-RRLYR-03541 is another candidate for RR Lyr in eclipsing binary (Soszyński et al 2009).…”

Section: Introductionmentioning

confidence: 99%

New analysis of the light time effect in TU Ursae Majoris

Liška

Skarka

Mikulášek

et al. 2016

A&A

View full text Add to dashboard Cite

Context. Recent statistical studies prove that the percentage of RR Lyrae pulsators that are located in binaries or multiple stellar systems is considerably lower than might be expected. This can be better understood from an in-depth analysis of individual candidates. We investigate in detail the light time effect of the most probable binary candidate TU UMa. This is complicated because the pulsation period shows secular variation. Aims. We model possible light time effect of TU UMa using a new code applied on previously available and newly determined maxima timings to confirm binarity and refine parameters of the orbit of the RRab component in the binary system. The binary hypothesis is also tested using radial velocity measurements. Methods. We used new approach to determine brightness maxima timings based on template fitting. This can also be used on sparse or scattered data. This approach was successfully applied on measurements from different sources. To determine the orbital parameters of the double star TU UMa, we developed a new code to analyse light time effect that also includes secular variation in the pulsation period. Its usability was successfully tested on CL Aur, an eclipsing binary with mass-transfer in a triple system that shows similar changes in the O-C diagram. Since orbital motion would cause systematic shifts in mean radial velocities (dominated by pulsations), we computed and compared our model with centre-of-mass velocities. They were determined using high-quality templates of radial velocity curves of RRab stars. Results. Maxima timings adopted from the GEOS database (168) together with those newly determined from sky surveys and new measurements (85) were used to construct an O-C diagram spanning almost five proposed orbital cycles. This data set is three times larger than data sets used by previous authors. Modelling of the O-C dependence resulted in 23.3-yr orbital period, which translates into a minimum mass of the second component of about 0.33 M . Secular changes in the pulsation period of TU UMa over the whole O-C diagram were satisfactorily approximated by a parabolic trend with a rate of −2.2 ms yr −1 . To confirm binarity, we used radial velocity measurements from nine independent sources. Although our results are convincing, additional long-term monitoring is necessary to unambiguously confirm the binarity of TU UMa.

show abstract

RR-Lyrae-type pulsations from a 0.26-solar-mass star in a binary system

Abstract: RR Lyrae pulsating stars have been extensively used as tracers of old stellar populations for the purpose of determining the ages of galaxies, and as tools to measure distances to nearby galaxies 1,2,3 . There was accordingly considerable

Cited by 111 publications

References 14 publications

The impact of large-scale, long-term optical surveys on pulsating star research

The impact of large-scale, long-term optical surveys on pulsating star research

Pulsating white dwarfs

New analysis of the light time effect in TU Ursae Majoris

Contact Info

Product

Resources

About