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Academic literature on the topic 'M-DWARF BINARY'

Author: Grafiati
Published: 10 December 2022
Last updated: 28 January 2023

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Journal articles on the topic "M-DWARF BINARY"

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Hogg, M. A., S. L. Casewell, G. A. Wynn, E. S. Longstaff, I. P. Braker, M. R. Burleigh, R. H. Tilbrook, et al. "Confirming new white dwarf-ultracool dwarf binary candidates." Monthly Notices of the Royal Astronomical Society 498, no. 1 (August 10, 2020): 12–24. http://dx.doi.org/10.1093/mnras/staa2233.

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ABSTRACT We present the results of a study to discover prospective new white dwarf-L dwarf binaries as identified by their near-infrared excesses in the UKIDSS catalogue. We obtained optical spectra to validate the white dwarf nature for 22 of the candidate primary stars, confirming ten as white dwarfs and determining their effective temperatures and gravities. For all 10 white dwarfs, we determined that the near-infrared excess was indeed indicative of a cool companion. Six of these are suggestive of late M dwarf companions, and three are candidate L dwarf companions, with one straddling the M−L boundary. We also present near-infrared spectra of eight additional candidate white dwarf-ultracool dwarf binaries, where the white dwarf primary had been previously confirmed. These spectra indicate one candidate at the M−L boundary, three potential L dwarf companions, and one suspected M dwarf, which showed photometric variability on a ∼6 h period, suggesting the system may be close. Radial velocity follow-up is required to confirm whether these systems are close, or widely separated.
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Han, Cheongho, Chung-Uk Lee, Yoon-Hyun Ryu, Doeon Kim, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, et al. "KMT-2019-BLG-0797: Binary-lensing event occurring on a binary stellar system." Astronomy & Astrophysics 649 (May 2021): A91. http://dx.doi.org/10.1051/0004-6361/202040149.

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Aims. We analyze the microlensing event KMT-2019-BLG-0797. The light curve of the event exhibits two anomalous features from a single-lens single-source model, and we aim to reveal the nature of the anomaly. Methods. It is found that a model with two lenses plus a single source (2L1S model) can explain one feature of the anomaly, but the other feature cannot be explained. We test various models and find that both anomalous features can be explained by introducing an extra source to a 2L1S model (2L2S model), making the event the third confirmed case of a 2L2S event, following MOA-2010-BLG-117 and OGLE-2016-BLG-1003. It is estimated that the extra source comprises ∼4% of the I-band flux from the primary source. Results. Interpreting the event is subject to a close–wide degeneracy. According to the close solution, the lens is a binary consisting of two brown dwarfs with masses (M1, M2) ∼ (0.034, 0.021) M⊙, and it is located at a distance of DL ∼ 8.2 kpc. According to the wide solution, on the other hand, the lens is composed of an object at the star–brown dwarf boundary and an M dwarf with masses (M1, M2) ∼ (0.06, 0.33) M⊙ located at DL ∼ 7.7 kpc. The source is composed of a late G dwarf to early K dwarf primary and an early-to-mid M dwarf companion.
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Landstreet, John D., and Stefano Bagnulo. "Discovery of a Sirius-like binary system with a very strongly magnetic white dwarf." Astronomy & Astrophysics 634 (February 2020): L10. http://dx.doi.org/10.1051/0004-6361/201937301.

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Non-interacting binary systems containing a magnetic white dwarf and a main-sequence star are considered extremely rare, perhaps non-existent. In the course of a search of magnetic fields in high-mass white dwarfs we have discovered a Sirius-like wide binary system composed of a main-sequence G0 star and an M ∼ 1.1 M⊙ white dwarf with a huge (hundreds of MG) magnetic field. This star, WDS J03038+0608B, shows a circular polarisation amplitude of 5% in the continuum, with no evidence of variability on a 1 d timescale, little or no linear polarisation in the blue part of the spectrum, and about 2% linear polarisation in the red part of the optical spectrum. A search in the literature reveals the existence of four more binary systems that include a magnetic white dwarf and a non-degenerate companion; three such systems passed unremarked in previous studies. We estimate that up to a few percent of magnetic white dwarfs may be found to occur in wide binary pairs. However, at least four of the five known binary systems with a magnetic white dwarf are too widely separated to be expected to evolve into systems experiencing Roche-lobe overflow, and cannot be considered as progenitors of magnetic cataclysmic variable (AM Her and DQ Her) systems.
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Wolz, Anna, Kent Yagi, Nick Anderson, and Andrew J. Taylor. "Measuring individual masses of binary white dwarfs with space-based gravitational-wave interferometers." Monthly Notices of the Royal Astronomical Society: Letters 500, no. 1 (November 15, 2020): L52—L56. http://dx.doi.org/10.1093/mnrasl/slaa183.

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ABSTRACT Unlike gravitational waves from merging black holes and neutron stars that chirp significantly over the observational period of ground-based detectors, gravitational waves from binary white dwarfs are almost monochromatic. This makes it extremely challenging to measure their individual masses. Here, we take a novel approach of using finite-size effects and applying certain universal relations to measure individual masses of binary white dwarfs using Laser Interferometer Space Antenna. We found quasi-universal relations among the mass, moment of inertia, and tidal deformability of a white dwarf that do not depend sensitively on the white dwarf composition. These relations allow us to rewrite the moments of inertia and tidal deformabilities in the waveform in terms of the masses. We then carried out a Fisher analysis to estimate how accurately one can measure the individual masses from the chirp mass and finite-size measurements. We found that the individual white dwarf masses can be measured with LISA for a 4-yr observation if the initial frequency is high enough (∼0.02 Hz) and either the binary separation is small (∼1 kpc) or the masses are relatively large (m ≳ 0.8 M⊙). This opens a new possibility of measuring individual masses of binary white dwarfs with space-based interferometers.
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Zheng, Ling-Lin, Wei-Min Gu, Mouyuan Sun, Zhi-Xiang Zhang, Tuan Yi, Jianfeng Wu, Junfeng Wang, et al. "A White Dwarf–Main-sequence Binary Unveiled by Time-domain Observations from LAMOST and TESS." Astrophysical Journal 936, no. 1 (August 29, 2022): 33. http://dx.doi.org/10.3847/1538-4357/ac853f.

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Abstract We report a single-lined white dwarf–main-sequence binary system, LAMOST J172900.17+652952.8, which is discovered by the Large Sky Area Multi-Object Fibre Spectroscopic Telescope (LAMOST)’s medium-resolution time-domain surveys. The radial-velocity semi-amplitude and orbital period of the optical visible star are measured by using follow-up observations with the Palomar 200 inch telescope and light curves from the Transiting Exoplanet Survey Satellite (TESS). Thus the mass function of the invisible candidate white dwarf is derived, f(M 2) = 0.120 ± 0.003 M ⊙. The mass of the visible star is measured based on a spectral energy distribution fitting, M 1 = 0.81 − 0.06 + 0.07 M ⊙ . Hence, the mass of its invisible companion is M 2 ≳ 0.63 M ⊙. The companion ought to be a compact object rather than a main-sequence star owing to the mass ratio q = M 2/M 1 ≳ 0.78 and the single-lined spectra. The compact object is likely to be a white dwarf if the inclination angle is not small, i ≳ 40°. By using the Galaxy Evolution Explorer (GALEX) near-UV flux, the effective temperature of the white dwarf candidate is constrained as T eff WD ≲ 12,000–13,500 K. It is difficult to detect white dwarfs which are outshone by their bright companions via single-epoch optical spectroscopic surveys. Therefore, optical time-domain surveys can play an important role in unveiling invisible white dwarfs and other compact objects in binaries.
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Creevey, O. L., G. F. Benedict, T. M. Brown, R. Alonso, P. Cargile, G. Mandushev, D. Charbonneau, et al. "A New Detached M Dwarf Eclipsing Binary." Astrophysical Journal 625, no. 2 (May 11, 2005): L127—L130. http://dx.doi.org/10.1086/431278.

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Wilson, R. E., C. A. Pilachowski, and Dirk Terrell. "THE M DWARF ECLIPSING BINARY CU CANCRI." Astrophysical Journal 835, no. 2 (February 1, 2017): 251. http://dx.doi.org/10.3847/1538-4357/835/2/251.

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Maxted, P. F. L., T. R. Marsh, L. Morales-Rueda, M. A. Barstow, P. D. Dobbie, M. R. Schreiber, V. S. Dhillon, and C. S. Brinkworth. "RX J2130.6+4710 - an eclipsing white dwarf-M-dwarf binary star." Monthly Notices of the Royal Astronomical Society 355, no. 4 (December 2004): 1143–54. http://dx.doi.org/10.1111/j.1365-2966.2004.08393.x.

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Rebassa-Mansergas, Alberto, Siyi Xu, Roberto Raddi, Anna F. Pala, Enrique Solano, Santiago Torres, Francisco Jiménez-Esteban, and Patricia Cruz. "Gaia 0007–1605: An Old Triple System with an Inner Brown Dwarf–White Dwarf Binary and an Outer White Dwarf Companion." Astrophysical Journal Letters 927, no. 2 (March 1, 2022): L31. http://dx.doi.org/10.3847/2041-8213/ac5a55.

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Abstract We identify Gaia 0007–1605 A,C as the first inner brown dwarf–white dwarf binary of a hierarchical triple system in which the outer component is another white dwarf (Gaia 0007–1605 B). From optical/near-infrared spectroscopy obtained at the Very Large Telescope with the X-Shooter instrument and/or from Gaia photometry plus spectral energy distribution fitting, we determine the effective temperatures and masses of the two white dwarfs (12,018 ± 68 K and 0.54 ± 0.01 M ⊙ for Gaia 0007–1605 A and 4445 ± 116 K and 0.56 ± 0.05 M ⊙ for Gaia 0007–1605 B) and the effective temperature of the brown dwarf (1850 ± 50 K; corresponding to spectral type L3 ± 1). By analyzing the available TESS light curves of Gaia 0007–1605 A,C we detect a signal at 1.0446 ± 0.0015 days with an amplitude of 6.25 ppt, which we interpret as the orbital period modulated from irradiation effects of the white dwarf on the brown dwarf’s surface. This drives us to speculate that the inner binary evolved through a common-envelope phase in the past. Using the outer white dwarf as a cosmochronometer and analyzing the kinematic properties of the system, we conclude that the triple system is about 10 Gyr old.
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Clark, Catherine A., Gerard T. van Belle, Elliott P. Horch, Kaspar von Braun, David R. Ciardi, Jennifer G. Winters, and Rocio Kiman. "The POKEMON Speckle Survey of Nearby M Dwarfs. I. New Discoveries." Astronomical Journal 164, no. 2 (July 4, 2022): 33. http://dx.doi.org/10.3847/1538-3881/ac739c.

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Abstract M dwarfs are favorable targets for exoplanet detection with current instrumentation, but stellar companions can induce false positives and inhibit planet characterization. Knowledge of stellar companions is also critical to our understanding of how binary stars form and evolve. We have therefore conducted a survey of stellar companions around nearby M dwarfs, and here we present our new discoveries. Using the Differential Speckle Survey Instrument at the 4.3 m Lowell Discovery Telescope, and the similar NN-EXPLORE Exoplanet Stellar Speckle Imager at the 3.5 m WIYN telescope, we carried out a volume-limited survey of M-dwarf multiplicity to 15 parsecs, with a special emphasis on including the later M dwarfs that were overlooked in previous surveys. Additional brighter targets at larger distances were included for a total sample size of 1070 M dwarfs. Observations of these 1070 targets revealed 26 new companions; 22 of these systems were previously thought to be single. If all new discoveries are confirmed, then the number of known multiples in the sample will increase by 7.6%. Using our observed properties, as well as the parallaxes and 2MASS K magnitudes for these objects, we calculate the projected separation, and estimate the mass ratio and component spectral types, for these systems. We report the discovery of a new M-dwarf companion to the white dwarf Wolf 672 A, which hosts a known M-dwarf companion as well, making the system trinary. We also examine the possibility that the new companion to 2MASS J13092185-2330350 is a brown dwarf. Finally, we discuss initial insights from the POKEMON survey.
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Dissertations / Theses on the topic "M-DWARF BINARY"

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Häuser, Marco [Verfasser], and Ralf [Akademischer Betreuer] Bender. "Radial velocity measurements for white-dwarf/brown-dwarf binarie candidates and development of an active mirror control for the 11 m Hobby-Eberly-Telescope / Marco Häuser ; Betreuer: Ralf Bender." München : Universitätsbibliothek der Ludwig-Maximilians-Universität, 2019. http://d-nb.info/1196529205/34.

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Häuser, Marco Verfasser], and Ralf [Akademischer Betreuer] [Bender. "Radial velocity measurements for white-dwarf/brown-dwarf binarie candidates and development of an active mirror control for the 11 m Hobby-Eberly-Telescope / Marco Häuser ; Betreuer: Ralf Bender." München : Universitätsbibliothek der Ludwig-Maximilians-Universität, 2019. http://d-nb.info/1196529205/34.

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Morgan, Dylan Parker. "The effects of close binaries on the magnetic activity of M dwarfs as probed using close white dwarf companions." Thesis, 2017. https://hdl.handle.net/2144/20874.

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I present a study of close white dwarf (WD) and M dwarf (dM) binary systems (WD+dM) to examine the effects that close companions have on the magnetic field generation in dMs. Using the Sloan Digital Sky Survey (SDSS) Data Release 8 spectroscopic database, I construct a sample of 1756 WD+dM high-quality pairs. I show that high-mass dMs (≤M4) in close binary systems are more likely to be magnetically active (as measured by Hα emission) and are able to remain active longer than field dMs. At lower masses (≥M5), where dMs become fully convective, the activity fraction and activity lifetimes of WD+dM binary systems become more comparable to those of the field dMs. The implications of having a close binary companion may include, increased stellar rotation through disk disruption, tidal effects, and/or angular momentum exchange. Thus, the similarity in activity between late-type field dMs and late-type dMs with close companions is likely due to the mechanism generating magnetic fields being less sensitive to the effects caused by a close companion; namely, increased stellar rotation. Using a subset of 181 close WD+dM pairs, matched to the time-domain SDSS Stripe 82 catalog, I show that enhanced magnetic activity extends to the flaring behavior of dMs in close binaries. Specifically, early spectral type dMs (M0-M1), in close WD+dM pairs, are two orders of magnitude more likely to flare than field dMs, whereas mid-type dMs (M2-M3) and late-type dMs (M4-M6) flare as frequently or less than the mid- to late-type field dM sample. To test whether the presence of a close companion leads to star-star interactions, I search for correlations between the WD occultations and flares from the dM member in KOI-256, an eclipsing WD+dM system from Kepler I find no correlations between the flaring activity of the dM and the WD occultations, indicating the there are no obvious signs of star-star interactions at work. In addition, the dM member of KOI-256 flares more than any other dM observed by Kepler and shows evidence for solar-like magnetic activity cycles, a feature not seen in many dMs to date.
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Conference papers on the topic "M-DWARF BINARY"

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Barry, R. K., B. O. Demory, D. Ségransan, T. Forveille, W. C. Danchi, E. Di Folco, D. Queloz, et al. "Ultra-precise Masses and Magnitudes for the Gliese 268 M-dwarf Binary." 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/10.1063/1.3099232.

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