Absolute Properties of the Pre-Main-Sequence Eclipsing Binary Star Np Persei

Lacy, Claud H.; Fekel, Francis C.; Pavlovski, K.; Torres, Guillermo; Muterspaugh, Matthew W.

doi:10.3847/0004-6256/152/1/2

Cited by 13 publications

(2 citation statements)

References 46 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…when the age of the secondary star is considered, the effective temperature of the primary is too high by about 700 K, making this hypothesis unlikely. Such discrepancies have already been reported by Lacy et al (2016) for another PMS eclipsing binary, namely NP Persei. In particular, the authors found that the two components of NP Per cannot be fitted at a single age, implying a relative age difference of about 44%.…”

Section: Evolutionary Status Of V1200 Censupporting

confidence: 59%

Analysis of eclipsing binaries in multiple stellar systems: the case of V1200 Centauri

Marcadon,

Hełminiak,

Marques

et al. 2020

Preprint

View full text Add to dashboard Cite

We present a new analysis of the multiple star V1200 Centauri based on the most recent observations for this system. We used the photometric observations from the Solaris network and the TESS telescope, combined with the new radial velocities from the CHIRON spectrograph and those published in the literature. We confirmed that V1200 Cen consists of a 2.5-day eclipsing binary orbited by a third body. We derived the parameters of the eclipsing components, which are M Aa = 1.393 ± 0.018 M , R Aa = 1.407 ± 0.014 R and T eff, Aa = 6 588 ± 58 K for the primary, and M Ab = 0.863 3±0.008 1 M , R Ab = 1.154±0.014 R and T eff, Ab = 4 475±68 K for the secondary. Regarding the third body, we obtained significantly different results than previously published. The period of the outer orbit is found to be 180.4 days, implying a minimum mass M B = 0.871 ± 0.020 M . Thus, we argue that V1200 Cen is a quadruple system with a secondary pair composed of two low-mass stars. Finally, we determined the ages of each eclipsing component using two evolution codes, namely MESA and CESTAM. We obtained ages of 16-18.5 Myr and 5.5-7 Myr for the primary and the secondary, respectively. In particular, the secondary appears larger and hotter than predicted at the age of the primary. We concluded that dynamical and tidal interactions occurring in multiples may alter the stellar properties and explain the apparent non-coevality of V1200 Centauri.

show abstract

Section: Evolutionary Status Of V1200 Censupporting

confidence: 59%

Analysis of eclipsing binaries in multiple stellar systems: the case of V1200 Centauri

Marcadon,

Hełminiak,

Marques

et al. 2020

Preprint

View full text Add to dashboard Cite

show abstract

“…At higher masses (>0.8 M ), J0552−0044 joins the intermediate age systems NP Per (1.3 + 1.0 M , ∼17 Myr; Lacy et al 2016), MML 53 (1.0 + 0.9 + 0.7 M , 16 Myr; Hebb et al 2010Hebb et al , 2011Gómez Maqueo Chew et al 2019) and several solar-type EBs in the greater Orion OB1 association (Stassun et al 2014). MML 53 in particular has a well-constrained age from its membership in the Upper Centaurus Lupus subgroup of the Sco-Cen OB association (16 ± 2 Myr; Pecaut & Mamajek 2016).…”

Section: J0552−0044 In Contextmentioning

confidence: 97%

THOR 42: A touchstone ∼24 Myr-old eclipsing binary spanning the fully-convective boundary

Murphy

Lawson

Onken

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present the characterization of CRTS J055255.7−004426 (=THOR 42), a young eclipsing binary comprising two pre-main sequence M dwarfs (combined spectral type M3.5). This nearby (103 pc), short-period (0.859 d) system was recently proposed as a member of the ∼24 Myr-old 32 Orionis Moving Group. Using ground-and space-based photometry in combination with medium-and high-resolution spectroscopy, we model the light and radial velocity curves to derive precise system parameters. The resulting component masses and radii are 0.497 ± 0.005 and 0.205 ± 0.002 M , and 0.659 ± 0.003 and 0.424 ± 0.002 R , respectively. With mass and radius uncertainties of ∼1 per cent and ∼0.5 per cent, respectively, THOR 42 is one of the most precisely characterized pre-main sequence eclipsing binaries known. Its systemic velocity, parallax, proper motion, colour-magnitude diagram placement and enlarged radii are all consistent with membership in the 32 Ori Group. The system provides a unique opportunity to test pre-main sequence evolutionary models at an age and mass range not well constrained by observation. From the radius and mass measurements we derive ages of 22-26 Myr using standard (non-magnetic) models, in excellent agreement with the age of the group. However, none of the models can simultaneously reproduce the observed mass, radius, temperature and luminosity of the coeval components. In particular, their H-R diagram ages are 2-4 times younger and we infer masses ∼50 per cent smaller than the dynamical values.

show abstract

Weighing stars from birth to death: mass determination methods across the HRD

Serenelli

Weiß

Aerts

et al. 2021

Astron Astrophys Rev

Self Cite

View full text Add to dashboard Cite

The mass of a star is the most fundamental parameter for its structure, evolution, and final fate. It is particularly important for any kind of stellar archaeology and characterization of exoplanets. There exist a variety of methods in astronomy to estimate or determine it. In this review we present a significant number of such methods, beginning with the most direct and model-independent approach using detached eclipsing binaries. We then move to more indirect and model-dependent methods, such as the quite commonly used isochrone or stellar track fitting. The arrival of quantitative asteroseismology has opened a completely new approach to determine stellar masses and to complement and improve the accuracy of other methods. We include methods for different evolutionary stages, from the pre-main sequence to evolved (super)giants and final remnants. For all methods uncertainties and restrictions will be discussed. We provide lists of altogether more than 200 benchmark stars with relative mass accuracies between ½0:3; 2% for the covered mass range of M 2 ½0:1; 16 M , 75% of which are stars burning hydrogen in their core and the other 25% covering all other evolved stages. We close with a recommendation how to combine various methods to arrive at a ''mass-ladder'' for stars.

show abstract

Absolute Properties of the Pre-Main-Sequence Eclipsing Binary Star Np Persei

Cited by 13 publications

References 46 publications

Analysis of eclipsing binaries in multiple stellar systems: the case of V1200 Centauri

Analysis of eclipsing binaries in multiple stellar systems: the case of V1200 Centauri

THOR 42: A touchstone ∼24 Myr-old eclipsing binary spanning the fully-convective boundary

Weighing stars from birth to death: mass determination methods across the HRD

Contact Info

Product

Resources

About