Geology of southeastern Canada

Poole, W H; Sanford, B. V.; Williams, Harold; Kelley, D G

doi:10.4095/106149

Cited by 32 publications

(8 citation statements)

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“…We have obtained high S/N low resolution spectra for Kelley & Shaw's (2007) proposed sdB+dM stars (their Table 3). All were observed with the same telescope and instrumental setup ( §3) that we used to obtain our initial spectrum of 2M 1533+3759.…”

Section: Nsvs Eclipsing Sdb+dm Candidatesmentioning

confidence: 99%

“…HW Vir and 2M 1533+3759 are therefore, unfortunately, the only two bonafide sdB stars in Kelley & Shaw's (2007) list. Figure 1 shows our flux-calibrated spectrum for 2M 1533+3759, along with the bluest and reddest of the non-sdB spectra from Table 3, for comparison.…”

Section: Nsvs Eclipsing Sdb+dm Candidatesmentioning

confidence: 99%

“…This star was first recognized as an sdB in 2005 (although it remained unpublished) during a continuing spectroscopic survey ) of bright blue stellar candidates selected from a variety of sources, including the 2MASS survey (Skrutskie et al 2006). The current investigation was motivated by Kelley & Shaw (2007), who discovered that 2M 1533+3759 is an eclipsing binary, NSVS 07826147, through their work with the Northern Sky Variability Survey (NSVS; Wozniak et al 2004). Kelley & Shaw (2007) identified a group of nine eclipsing binaries with short periods and relatively narrow eclipse widths, indicating very small radii for the components.…”

Section: Introductionmentioning

confidence: 99%

“…The current investigation was motivated by Kelley & Shaw (2007), who discovered that 2M 1533+3759 is an eclipsing binary, NSVS 07826147, through their work with the Northern Sky Variability Survey (NSVS; Wozniak et al 2004). Kelley & Shaw (2007) identified a group of nine eclipsing binaries with short periods and relatively narrow eclipse widths, indicating very small radii for the components. Since their list includes the well-known HW Vir (Lee et al 2009 and references therein), as well as 2M 1533+3759, which we confirmed to be a spectroscopic near-twin of HW Vir, Kelley & Shaw (2007) proposed that the other objects in their Table 3 might also be sdB+dM binaries.…”

Section: Introductionmentioning

confidence: 99%

“…Kelley & Shaw (2007) identified a group of nine eclipsing binaries with short periods and relatively narrow eclipse widths, indicating very small radii for the components. Since their list includes the well-known HW Vir (Lee et al 2009 and references therein), as well as 2M 1533+3759, which we confirmed to be a spectroscopic near-twin of HW Vir, Kelley & Shaw (2007) proposed that the other objects in their Table 3 might also be sdB+dM binaries. §2 presents the results from our follow-up spectra for these stars.…”

Section: Introductionmentioning

confidence: 99%

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MODELING THE SYSTEM PARAMETERS OF 2M 1533+3759: A NEW LONGER PERIOD LOW-MASS ECLIPSING sdB+dM BINARY

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Green

Fontaine

et al. 2009

ApJ

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We present new photometric and spectroscopic observations for 2M 1533+3759 (= NSVS 07826147), the seventh eclipsing subdwarf B star + M dwarf (sdB+dM) binary ever found. It has an orbital period of 0.16177042 day, or ∼3.88 h, significantly longer than the 2.3-3.0 hour periods of the other known eclipsing sdB+dM systems. Spectroscopic analysis of the hot primary yields T eff = 29230 ± 125 K, log g = 5.58 ± 0.03 and log N(He)/N(H) = −2.37 ± 0.05. The sdB velocity amplitude is K 1 = 71.1 ± 1.0 km s −1 . The only detectable light contribution from the secondary is due to the surprisingly strong reflection effect, whose peak-to-peak BV RI amplitudes are 0.10, 0.13, 0.15, and 0.19 magnitudes, respectively. Light curve modeling produced several solutions corresponding to different values of the system mass ratio, q (M 2 /M 1 ), but only one is consistent with a core helium burning star, q = 0.301. The -2orbital inclination is 86.6 • . The sdB primary mass is M 1 = 0.376 ± 0.055 M ⊙ and its radius is R 1 = 0.166 ± 0.007 R ⊙ . 2M 1533+3759 joins PG 0911+456 (and possibly also HS 2333+3927) in having an unusually low mass for an sdB star. SdB stars with masses significantly lower than the canonical value of 0.48 M ⊙ , down to as low as 0.30 M ⊙ , were theoretically predicted by Han et al. (2002Han et al. ( , 2003, but observational evidence has only recently begun to confirm the existence of such stars. The existence of core helium burning stars with masses lower than 0.40-0.43 M ⊙ implies that at least some sdB progenitors have initial main sequence masses of 1.8-2.0 M ⊙ or more, i.e. they are at least main sequence A stars. The orbital separation in 2M 1533+3759 is a = 0.98 ± 0.04 R ⊙ . The secondary has M 2 = 0.113 ± 0.017 M ⊙ , R 2 = 0.152 ± 0.005 R ⊙ and T eff 2 = 3100 ± 600 K, consistent with a main sequence M5 star. If 2M 1533+3759 becomes a cataclysmic variable (CV), its orbital period will be 1.6 h, below the CV period gap.

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Section: Nsvs Eclipsing Sdb+dm Candidatesmentioning

confidence: 99%

Section: Nsvs Eclipsing Sdb+dm Candidatesmentioning

confidence: 99%