Tootfinder

An Eccentric Planet Orbiting the Polar V808 Aurigae
McKenna Leichty, Peter Garnavich, Colin Littlefield, Axel D. Schwope, Jan Kurpas, Paul A. Mason, Klaus Beuermann
https://arxiv.org/abs/2402.16959

An Eccentric Planet Orbiting the Polar V808 Aurigae
We analyze 15 years of eclipse timings of the polar V808 Aur. The rapid ingress/egress of the white dwarf and bright accretion region provide timings as precise as a few tenths of a second for rapid cadence photometric data. We find that between 2015 and 2018, the eclipse timings deviated from a linear ephemeris by more than 30 s. The rapid timing change is consistent with the periastron passage of a planet in an eccentric orbit about the polar. The best fit orbital period is 11$\pm 1$ yr and w…

This https://arxiv.org/abs/2404.04013 has been replaced.
initial toot: https://mastoxiv.page/@arXiv_grqc_…

Tidal heating as a discriminator for horizons in equatorial eccentric extreme mass ratio inspirals
Tidal heating in a binary black hole system is driven by the absorption of energy and angular momentum by the black hole's horizon. Previous works have shown that this phenomenon becomes particularly significant during the late stages of an extreme mass ratio inspiral (EMRI) into a rapidly spinning massive black hole, a key focus for future low-frequency gravitational-wave observations by (for instance) the LISA mission. Past analyses have largely focused on quasi-circular inspiral geometry, wi…

Decretion disc size in Be/X-ray binaries depends upon the disc aspect ratio
Rebecca G. Martin, Stephen H. Lubow, Philip J. Armitage, Daniel J. Price
https://arxiv.org/abs/2404.17976

Decretion disc size in Be/X-ray binaries depends upon the disc aspect ratio
With three-dimensional hydrodynamical simulations we show that the size of the decretion disc and the structure of the accretion flow onto the neutron star in a Be/X-ray binary strongly depends upon the disc aspect ratio, $H/R$. We simulate a Be star disc that is coplanar to the orbit of a circularly or moderately eccentric neutron star companion, thereby maximising the effects of tidal truncation. For low disc aspect ratio, $H/R\lesssim 0.1$, the disc is efficiently tidally truncated by the ne…

(Not sure what the appropriate comment is - but this is a good thing)
https://www.theguardian.com/uk-news/2024/mar/27/yorkshire-estate-known-as-worlds-first-nature-r…

(Not sure what the appropriate comment is - but this is a good thing)
https://www.theguardian.com/uk-news/2024/mar/27/yorkshire-estate-known-as-worlds-first-nature-r…

This https://arxiv.org/abs/2402.13053 has been replaced.
initial toot: https://mastoxiv.page/@arXiv_grqc_…

Sharpening the dark matter signature in gravitational waveforms I: Accretion and eccentricity evolution
Dark matter overdensities around black holes can alter the dynamical evolution of a companion object orbiting around it, and cause a dephasing of the gravitational waveform. Here, we present a refined calculation of the co-evolution of the binary and the dark matter distribution, taking into account the accretion of dark matter particles on the companion black hole, and generalizing previous quasi-circular calculations to the general case of eccentric orbits. These calculations are validated by…

This https://arxiv.org/abs/2211.12026 has been replaced.
link: https://scholar.google.com/scholar?q=a

Repeating fast radio bursts produced by a strange star interacting with its planet in an eccentric orbit
FRB 180916 is an important repeating fast radio burst (FRB) source. Interestingly, the activity of FRB 180916 shows a well-regulated behavior, with a period of 16.35 days. The bursts are found to occur in a duty circle of about 5 days in each period. In this study, we suggest that the bursts of FRB 180916 are produced by a strange star interacting with its planet. The planet moves in a highly eccentric orbit around its compact host, with the periastron only slightly beyond the tidal disruption …

Six new eccentric eclipsing systems with a third body
P. Zasche, Z. Henzl, M. Wolf
https://arxiv.org/abs/2403.16657 https://arxiv.org…

Six new eccentric eclipsing systems with a third body
We present the discovery of six new triple stellar system candidates composed of an inner eccentric-orbit eclipsing binary with an apsidal motion. These stars were studied using new, precise TESS light curves and a long-term collection of older photometric ground-based data. These data were used for the monitoring of ETVs (eclipse timing variations) and to detect the slow apsidal movements along with additional periodic signals. The systems analysed were ASASSN-V J012214.37+643943.3 (orbital pe…

A study of the Inspiral-Merger-Ringdown Consistency Test with gravitational-wave signals from compact binaries in eccentric orbits
Md Arif Shaikh, Sajad A. Bhat, Shasvath J. Kapadia
https://arxiv.org/abs/2402.15110

A study of the Inspiral-Merger-Ringdown Consistency Test with gravitational-wave signals from compact binaries in eccentric orbits
The Inspiral Merger Ringdown Consistency Test (IMRCT) is one among a battery of tests of general relativity (GR) employed by the LIGO-Virgo-KAGRA (LVK) collaboration. It is used to search for deviations from GR in detected gravitational waves (GWs) from compact binary coalescences (CBCs) in a model-agnostic way. The test compares source parameter estimates extracted independently from the inspiral and post-inspiral portions of the CBC signals and, therefore, crucially relies on the accurate mod…

This https://arxiv.org/abs/2401.12889 has been replaced.
initial toot: https://mastoxiv.page/@arXiv_…

Is PSR J0514$-$4002E in a PBH-NS binary?
Recent pulsar timing observations using MeerKAT of the eccentric binary millisecond pulsar, PSR J0514$-$4002E, have unveiled a companion with a mass in the mass gap, ranging from $2.09\, M_\odot$ to $2.71\, M_\odot$. This challenges conventional astrophysical scenarios for black hole formation. In this letter, we present an alternative explanation: PSR J0514$-$4002E could be in a PBH-NS binary, with the companion potentially being a primordial black hole formed during the early Universe's first…