Visual Binaries for the Mass-Luminosity Relation.

Strand, K. Aa.; Hall, R. G.

doi:10.1086/145917

Cited by 10 publications

(3 citation statements)

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“…Throughout the century it has been revised, updated and improved upon as newer and more accurate data became available. Among the many authors contributing to those revisions, some of the most notable include Eddington (1926), McLaughlin (1927), Kuiper (1938), Petrie (1950a,b), Strand & Hall (1954), Eggen (1956), Popper (1967Popper ( , 1980, McCluskey & Kondo (1972), Heintz (1978), Cester, Ferluga & Boehm (1983), Griffiths, Hicks, & Milone (1988), Henry & McCarthy (1993), Demircan & Kahraman (1991), Andersen (1991), Gorda & Svechnikov (1998), Ibanoǧlu et al (2006), Malkov (2007), Torres, Andersen & Giménez (2010) and Gafeira, Patacas (2012). Recently, Eker et al (2015), Benedict et al (2016) and Moya et al (2018) have also contributed to those revisions.…”

Section: Introductionmentioning

confidence: 99%

Interrelated main-sequence mass–luminosity, mass–radius, and mass–effective temperature relations

Eker

Bakış

Bilir

et al. 2018

Monthly Notices of the Royal Astronomical Society

216

185

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Absolute parameters of 509 main-sequence stars selected from the components of detached-eclipsing spectroscopic binaries in the Solar neighbourhood are used to study mass-luminosity, mass-radius and mass-effective temperature relations (MLR, MRR and MTR). The MLR function is found better if expressed by a six-piece classical MLR (L ∝ M α ) rather than a fifth or a sixth degree polynomial within the mass range of 0.179 M/M ⊙ 31. The break points separating the mass-ranges with classical MLR do not appear to us to be arbitrary. Instead, the data indicate abrupt changes along the mass axis in the mean energy generation per unit of stellar mass. Unlike the MLR function, the MRR and MTR functions cannot be determined over the full range of masses. A single piece MRR function is calibrated from the radii of stars with M 1.5M ⊙ , while a second single piece MTR function is found for stars with M > 1.5M ⊙ . The missing part of the MRR is computed from the MLR and MTR, while the missing part of the MTR is computed from the MLR and MRR. As a result, we have interrelated MLR, MRR and MTR, which are useful in determining the typical absolute physical parameters of main-sequence stars of given masses. These functions are also useful to esc The Authors 2 Eker et al. timate typical absolute physical parameters from typical T ef f values. Thus, we were able to estimate the typical absolute physical parameters of mainsequence stars observed in the Sejong Open Cluster survey, based on that survey's published values for T ef f . Since typical absolute physical parameters of main sequence stars cannot normally be determined in such photometric surveys, the interrelated functions are shown to be useful to compute such missing parameters from similar surveys.

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Section: Introductionmentioning

confidence: 99%

Interrelated main-sequence mass–luminosity, mass–radius, and mass–effective temperature relations

Eker

Bakış

Bilir

et al. 2018

Monthly Notices of the Royal Astronomical Society

216

185

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“…Investigations of the MLR continued as the quantity and quality of data increased (Kuiper 1938;Petrie 1950a,b;Strand & Hall 1954;Eggen 1956;Cester, Ferluga & Boehm 1983;Henry & McCarthy 1993). Especially noteworthy was the critical compilation of absolute dimensions of binary components by Popper (1967Popper ( , 1980.…”

Section: Introductionmentioning

confidence: 99%

Main-Sequence Effective Temperatures From a Revised Mass–luminosity Relation Based on Accurate Properties

et al. 2015

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The mass-luminosity (M − L), mass-radius (M − R) and mass-effective temperature (M − T ef f ) diagrams for a subset of galactic nearby main-sequence stars with masses and radii accurate to ≤ 3% and luminosities accurate to ≤ 30% (268 stars) has led to a putative discovery. Four distinct mass domains have been identified, which we have tentatively associated with low, intermediate, high, and very high mass main-sequence stars, but which nevertheless are clearly separated by three distinct break points at 1.05, 2.4, and 7M ⊙ within the mass range studied of 0.38 − 32M ⊙ . Further, a revised mass-luminosity relation (MLR) is found based on linear fits for each of the mass domains identified. The revised, mass-domain based MLRs, which are classical (L ∝ M α ), are shown to be preferable to a single linear, quadratic or cubic equation representing as an alternative MLR. Stellar radius evolution within the main-sequence for stars with M > 1M ⊙ is clearly evident on the M − R diagram, but it is not the clear on the M − T ef f diagram based on published temperatures. Effective temperatures can be calculated directly using the well-known Stephan-Boltzmann law by employing the accurately known values of M and R with the newly defined MLRs. With the calculated temperatures, stellar temperature evolution within the main-sequence for stars with M > 1M ⊙ is clearly visible on the M − T ef f diagram.Our study asserts that it is now possible to compute the effective temperature of a mainsequence star with an accuracy of ∼ 6%, as long as its observed radius error is adequately small (< 1%) and its observed mass error is reasonably small (< 6%).A calibration sample was formed by selecting main-sequence stars with the most accurate masses, radii and effective temperatures from Table 2 of "The Catalogue of Stellar Parameters ..." by Eker et al. (2014), which is already reprocessed and homogenized. In the first step, our preliminary criteria involved finding stars where both mass and radius with errors of less than or equal to 3%, and luminosities with errors less than or equal to 30% were available. Among 514 stars (257 binaries), 296 stars were found fulfilling the criteria.In the second step, 25 stars outside of the main sequence were removed.The process of removing non-main-sequence stars was completed by using the mass-radius diagram. Compared to effective temperatures and luminosities, which can only be inferred indirectly, masses and radii provide much more reliable indicators of stellar properties, and a highly improved diagnostic tool for analyzing stellar evolution. Fig. 1 shows 271 main-sequence stars selected for the calibration sample and 25 non main-sequence stars on the M − R diagram. Theoretical ZAMS (Zero Age Main Sequence) and TAMS (Terminal Age Main Sequence) lines for metallicity zero from Bertelli et al. (2008Bertelli et al. ( , 2009 were used as border lines to secure the stars within the main-sequence band.Although metallicity data is missing in the catalogue of Eker et al. (2014), the thin-disk field stars in ...

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“…The main-sequence mass-luminosity relation (MLR) was discovered independently by Hertzsprung (1923) and Russell, Adams & Joy (1923) empirically in the middle of the first half of the 20th century. As newer and more accurate data came along, it has been revised, updated and improved (Eddington 1926;McLaughlin 1927;Kuiper 1938a;Petrie 1950a,b;Strand & Hall 1954;Eggen 1956;McCluskey & Kondo 1972;Cester, Ferluga & Boehm 1983;Griffiths, Hicks, & Milone 1988;Demircan & Kahraman 1991) many times. Early relations were demonstrated as mass-absolute bolometric magnitude diagrams, some with the best fitting curve and some without.…”

Section: Mass-luminosity Relations For Predicting Lmentioning

confidence: 99%

Standard stellar luminosities; what are typical and limiting accuracies in the era after Gaia?

Eker,

Soydugan,

Bilir

et al. 2021

Preprint

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Methods of obtaining stellar luminosities (𝐿) have been revised and a new concept, standard stellar luminosity, has been defined. Among the three methods (direct method from radii and effective temperatures, method using a mass-luminosity relation (MLR) and method requiring a bolometric correction), the third method, which uses the unique bolometric correction (BC) of a star extracted from a flux ratio ( 𝑓 V / 𝑓 Bol ) obtained from the observed spectrum with sufficient spectral coverage and resolution, is estimated to provide an uncertainty (Δ𝐿/𝐿) typically at a low percentage, which could be as accurate as 1% perhaps more. The typical and limiting uncertainties of the predicted 𝐿 of the three methods were compared. The secondary methods requiring either a pre-determined non-unique BC or MLR were found to provide less accurate luminosities than the direct method, which could provide stellar luminosities with a typical accuracy of 8.2% -12.2% while its estimated limiting accuracy is 2.5%.

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Visual Binaries for the Mass-Luminosity Relation.

Cited by 10 publications

References 0 publications

Interrelated main-sequence mass–luminosity, mass–radius, and mass–effective temperature relations

Interrelated main-sequence mass–luminosity, mass–radius, and mass–effective temperature relations

Main-Sequence Effective Temperatures From a Revised Mass–luminosity Relation Based on Accurate Properties

Standard stellar luminosities; what are typical and limiting accuracies in the era after Gaia?

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