Mass Transfer in Binary Stellar Evolution and Its Stability

Negu, Seblu Humne; Tessema, Solomon Belay

doi:10.4236/ijaa.2015.53026

Cited by 7 publications

(12 citation statements)

References 6 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Subsequently, using the orbital parameters of these catalogs, we calculate a and the actual Roche lobe radius r Ld for less and more massive donor stars using Equations , and the stellar parameters to construct the M − L , M − R , M − a relations using Equations . We also determine the stable mass transfer (Negu & Tessema ) in these systems with mass ratio q < 0.8.…”

Section: Statistical Analysis Of Algol‐type Eclipsing Systemsmentioning

confidence: 99%

Statistical analysis of Algol‐type eclipsing binaries with stable mass transfer

Negu

Tessema

2018

Astron Nachr

View full text Add to dashboard Cite

In this study, we have investigated the stellar parameters of Algol-type eclipsing binaries in the range of primary and secondary masses between 0.2 and 8 M ⊙ , which were obtained from the catalog of approximate photometric and absolute elements of eclipsing variable stars. We examined those parameters for classical Algols and hot semidetached binaries. We have made a statistical analysis of Algol-type eclipsing binaries' stellar parameters and constructed the mass-luminosity and mass-radius relations for the primary and secondary components of classical Algols and hot semidetached binaries.

show abstract

Section: Statistical Analysis Of Algol‐type Eclipsing Systemsmentioning

confidence: 99%

Statistical analysis of Algol‐type eclipsing binaries with stable mass transfer

Negu

Tessema

2018

Astron Nachr

View full text Add to dashboard Cite

show abstract

“…As we have investigated in [12], as the matter is being transferred between the 2 Throughout this paper, the subscripts "a" and "d" will correspond to the accretor and donor, respectively. International Journal of Astronomy and Astrophysics components in the binary systems, not only the mass ratio, q, but also the P orb will be changed due to angular momentum redistribution between the components of two stars.…”

Section: Evolution Of Angular Momentummentioning

confidence: 99%

“…As we investigated the rate of change of orbital angular momentum in Section (2.3), we develop the equations for the evolution of orbital period and the rotational angular velocities of the stars. It follows from Equation 3and [12] that ( )…”

Section: Differential Equations For the Evolution Of Orbital Parametersmentioning

confidence: 99%

“…As we have showed in [12] henceforth called paper I that mass transfer phase in binary stellar evolution can either decrease or increase the orbital period of the system, crucially depending on the exchange of angular momentum between the binary components, the orbit and the component spins. In order to calculate the angular momentum changes during mass transfer, both the studies of [9] and [10] utilize a numerical prescription based on [13] approximations to more accurately determine the flow of angular momentum between the component spins and the orbit.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Evolution of Angular Momentum and Orbital Period Changes in Close Double White Dwarf Binaries

Negu¹,

Tessema²

2018

IJAA

Self Cite

View full text Add to dashboard Cite

We have presented the evolution of angular momentum and orbital period changes between the component spins and the orbit in close double white dwarf binaries undergoing mass transfer through direct impact accretion over a broad range of orbital parameter space. This work improves upon similar earlier studies in a number of ways: First, we calculate self-consistently the angular momentum of the orbit at all times. This includes gravitational, tides and mass transfer effects in the orbital evolution of the component structure models, and allow the Roche lobe radius of the donor star and the rotational angular velocities of both components to vary, and account for the exchange of angular momentum between the spins of the white dwarfs and the orbit. Second, we investigate the mass transfer by modeling the ballistic motion of a point mass ejected from the center of the donor star through the inner Lagrangian point. Finally, we ensure that the angular momentum is conserved, which requires the donor star spin to vary self-consistently. With these improvements, we calculate the angular momentum and orbital period changes of the orbit and each binary component across the entire parameter space of direct impact double white dwarf binary systems. We find a significant decrease in the amount of angular momentum removed from the orbit during mass transfer, as well as cases where this process increases the angular momentum and orbital period of the orbit at the expense of the spin angular momentum of the donor and accretor. We find that our analysis yields an increase in the predicted number of stable systems compared to that in the previous studies, survive the onset of mass transfer, even if this mass transfer is initially unstable. In addition, as a consequence of the tidal coupling, systems that come into contact near the mass transfer instability boundary undergo a phase of mass transfer with their orbital period.

show abstract

“…The young embedded cluster NGC 6618 is thought to be younger than 3 Myr (Jiang et al 2002), and contains hundreds of stars earlier than B9 (Lada et al 1991;Hoffmeister et al 2008). M17 has been studied in depth from various aspects, such as physical properties of massive young stellar objects (MYSOs; Chini et al 2004;Nielbock et al 2007;Ramírez-Tannus et al 2017;Lim et al 2020;Chen et al 2021), magnetic fields of the H II region and surrounding molecular clouds (Chen et al 2012), the molecular gas distribution and overall star formation activities (Povich et al 2009;Nguyen-Luong et al 2020). As the mid-IR surveys like GLIMPSE and MIPSGAL covered the Galactic plane, an infrared dark cloud (IRDC) located southwest to M17 came into common interest.…”

Section: Introductionmentioning

confidence: 99%

New Massive Contact Twin Binary in a Radio-quiet HII Region Associated with the M17 Complex

Yin,

Chen,

Yao

et al. 2022

Preprint

View full text Add to dashboard Cite

Early-B stars, much less energetic than O stars, may create an H II region that appears as radio-quiet. We report the identification of new early-B stars associated with the radio-quiet H II region G014.645-00.606 in the M17 complex. The ratio-quiet H II region G014.645-00.606 is adjacent to three radio-quiet WISE H II region candidates (Anderson et al. 2014). The ionizing sources of the radio-quiet H II regions are expected to later than B1V, given the sensitivity about 1 − 2 mJy of the MAGPIS 20 cm survey. The stars were first selected if their parallaxes of GAIA EDR3 match that of the 22 GHz H 2 O maser source within the same region. We used the color-magnitude diagram made from the ZTF photometric catalog to select the candidates for massive stars because the intrinsic g − r colors of massive stars change little from B-type to O-type stars. Five stars lie in the areas of the color-magnitude diagram where either reddened massive stars or evolved post-main sequence stars of lower masses are commonly found. Three of the five stars, sources 1, 2, and 3, are located at the cavities of the three IR bubbles, and extended Hα emission is detected around the three IR bubbles. We suggest that sources 1, 2, and 3 are candidates for early-B stars associated with the radio-quiet region G014.645-00.606. Particularly, source 1 is an EW type eclipsing binary with a short period of 0.825 day, while source 2 is an EA type eclipsing binary with a short period of 0.919 day. The physical parameters of the two binary systems have been derived through the PHOEBE model. Source 1 is a twin binary of two stars with T eff ≈ 23, 500 K, and source 2 contains a hotter component (T eff ≈ 20, 100 K) and a cooler one (T eff ≈ 15, 500 K). The O − C values of source 1 show a trend of decline, implying that the period of source is deceasing. Source 1 is likely a contacting early-B twin binary, for which mass transfer might cause its orbit to shrink.

show abstract

Mass Transfer in Binary Stellar Evolution and Its Stability

Cited by 7 publications

References 6 publications

Statistical analysis of Algol‐type eclipsing binaries with stable mass transfer

Statistical analysis of Algol‐type eclipsing binaries with stable mass transfer

Evolution of Angular Momentum and Orbital Period Changes in Close Double White Dwarf Binaries

New Massive Contact Twin Binary in a Radio-quiet HII Region Associated with the M17 Complex

Contact Info

Product

Resources

About