Exhaust Emission Control on the New 500 SL and 500 SL Structure and Mode of Operation

Zahn, W.; Glese, Jost; Karl, Weining Hans

doi:10.4271/891973

Cited by 10 publications

(22 citation statements)

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“…These three changes take place on timescales much shorter than the lifetime of the binary (see e.g. Zahn 1977;Tassoul 1988). Thus, the rotational broadening of the star, projected onto our line-of-sight, is v rot sin i ≈ K 2 (1 + q)R 2 /a, where i is the binary inclination, K 2 the radial velocity semi-amplitude of the donor star and R 2 /a the ratio between the Roche-lobe effective radius of the donor star and the separation between the stellar components.…”

Section: Projected Rotational Velocity and Binary Mass Ratiomentioning

confidence: 99%

The Binary Mass Ratio in the Black Hole Transient MAXI J1820+070

Torres

Casares

Jiménez-Ibarra

et al. 2020

ApJL

119

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We present intermediate resolution spectroscopy of the optical counterpart to the black hole X-ray transient MAXI J1820+070 (=ASASSN-18ey) obtained with the OSIRIS spectrograph on the 10.4-m Gran Telescopio Canarias. The observations were performed with the source close to the quiescent state and before the onset of renewed activity in August 2019. We make use of these data and K-type dwarf templates taken with the same instrumental configuration to measure the projected rotational velocity of the donor star. We find v rot sin i = 84±5 km s −1 (1−σ), which implies a donor to black-hole mass ratio q = M 2 /M 1 = 0.072 ± 0.012 for the case of a tidally locked and Roche-lobe filling donor star. The derived dynamical masses for the stellar components are M 1 = (5.95 ± 0.22) sin −3 i M and M 2 = (0.43 ± 0.08) sin −3 i M . The use of q, combined with estimates of the accretion disk size at the time of the optical spectroscopy, allows us to revise our previous orbital inclination constraints to 66 • < i < 81 • . These values lead to 95% confidence level limits on the masses of 5.73 < M 1 (M ) < 8.34 and 0.28 < M 2 (M ) < 0.77. Adopting instead the 63 ± 3 • orientation angle of the radio jet as the binary inclination leads to M 1 = 8.48 +0.79 −0.72 M and M 2 = 0.61 +0.13 −0.12 M (1−σ).

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Section: Projected Rotational Velocity and Binary Mass Ratiomentioning

confidence: 99%

The Binary Mass Ratio in the Black Hole Transient MAXI J1820+070

Torres

Casares

Jiménez-Ibarra

et al. 2020

ApJL

119

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“…valid assumption since the synchronization timescale is 10 4 yr at the orbital period of J2333 (Zahn 1977).…”

Section: Modeling the Light Curvesmentioning

confidence: 99%

A New Likely Redback Millisecond Pulsar Binary with a Massive Neutron Star: 4FGL J2333.1–5527

Swihart

Strader

Urquhart

et al. 2020

ApJ

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We present the discovery of a likely new redback millisecond pulsar binary associated with the Fermi γ-ray source 4FGL J2333.1-5527. Using optical photometric and spectroscopic observations from the SOAR telescope, we identify a low-mass, main sequence-like companion in a 6.9-hr, highly inclined orbit around a suspected massive neutron star primary. Archival XMM-Newton X-ray observations show this system has a hard power-law spectrum Γ = 1.6 ± 0.3 and L X ∼ 5 × 10 31 erg s −1 , consistent with redback millisecond pulsar binaries. Our data suggest that for secondary masses typical of redbacks, the mass of the neutron star is likely well in excess of ∼ 1.4 M , but future timing of the radio pulsar is necessary to bolster this tentative conclusion. This work shows that a bevy of nearby compact binaries still await discovery, and that unusually massive neutron stars continue to be common in redbacks.

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“…Mustill & Villaver (2012) carried out detailed numerical simulations which determined the critical engulfment distance of different types of planets (different masses and compositions) around asymptotic giant branch stars whose main-sequence progenitor masses went up to 5M⊙. They used the equilibrium tidal model of Zahn (1977) for their formalism. Adams & Bloch (2013) instead took a different approach, and derived an analytical formula for the critical engulfment distance, deng, as a function of several free parameters.…”

Section: Orbital Engulfment Due To Tidal Interactionsmentioning

confidence: 99%

Constraining planet formation around 6–8 M⊙ stars

Veras

Tremblay

Hermes

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Identifying planets around O-type and B-type stars is inherently difficult; the most massive known planet host has a mass of only about 3M ⊙ . However, planetary systems which survive the transformation of their host stars into white dwarfs can be detected via photospheric trace metals, circumstellar dusty and gaseous discs, and transits of planetary debris crossing our line-of-sight. These signatures offer the potential to explore the efficiency of planet formation for host stars with masses up to the corecollapse boundary at ≈ 8M ⊙ , a mass regime rarely investigated in planet formation theory. Here, we establish limits on where both major and minor planets must reside around ≈ 6M ⊙ − 8M ⊙ stars in order to survive into the white dwarf phase. For this mass range, we find that intact terrestrial or giant planets need to leave the main sequence beyond approximate minimum star-planet separations of respectively about 3 and 6 au. In these systems, rubble pile minor planets of radii 10, 1.0, and 0.1 km would have been shorn apart by giant branch radiative YORP spin-up if they formed and remained within, respectively, tens, hundreds and thousands of au. These boundary values would help distinguish the nature of the progenitor of metal-pollution in white dwarf atmospheres. We find that planet formation around the highest mass white dwarf progenitors may be feasible, and hence encourage both dedicated planet formation investigations for these systems and spectroscopic analyses of the highest mass white dwarfs.

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Exhaust Emission Control on the New 500 SL and 500 SL Structure and Mode of Operation

Cited by 10 publications

References 0 publications

The Binary Mass Ratio in the Black Hole Transient MAXI J1820+070

The Binary Mass Ratio in the Black Hole Transient MAXI J1820+070

A New Likely Redback Millisecond Pulsar Binary with a Massive Neutron Star: 4FGL J2333.1–5527

Constraining planet formation around 6–8 M⊙ stars

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