Orbital Parameter Determination for Wide Stellar Binary Systems in the Age of Gaia

Pearce, Logan; Kraus, Adam L.; Dupuy, Trent J.; Mann, Andrew W.; Newton, Elisabeth R.; Tofflemire, Benjamin M.; Vanderburg, Andrew

doi:10.3847/1538-4357/ab8389

Cited by 44 publications

(41 citation statements)

References 86 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Triple System Orbit Analysis We investigated the orbits of the three stellar components in the WD 1856 system of WD 1856 and G 229-20 A/B about the system's center of mass. Gaia DR2 measured highly precise positions and proper motions for the three stars, so we used the Linear Orbits for the Impatient (LOFTI 77 ) algorithm 78 to derive orbital constraints from these observations. Given input proper motions, positions, radial velocities (if available), and masses of the stellar components, LOFTI uses rejection sampling 79 to determine probability distributions for different orbital parameters.…”

Section: Spitzer Observationsmentioning

confidence: 99%

A giant planet candidate transiting a white dwarf

Vanderburg

Rappaport

et al. 2020

Nature

Self Cite

183

101

View full text Add to dashboard Cite

Astronomers have discovered thousands of planets outside the solar system 1 , most of which orbit stars that will eventually evolve into red giants and then into white dwarfs. During the red giant phase, any close-orbiting planets will be engulfed by the star 2 , but more distant planets can survive this phase and remain in orbit around the white dwarf 3,4 . Some white dwarfs show evidence for rocky material floating in their atmospheres 5 , in warm debris disks [6][7][8][9] , or orbiting very closely [10][11][12] , which has been interpreted as the debris of rocky planets that were scattered inward and tidally disrupted 13 . Recently, the discovery of a gaseous debris disk with a composition similar to ice giant planets 14 demonstrated that massive planets might also find their way into tight orbits around white dwarfs, but it is unclear whether the planets can survive the journey. So far, the detection of intact planets in close orbits around white dwarfs has remained elusive. Here, we report the discovery of a giant planet candidate transiting the white dwarf WD 1856+534 (TIC 267574918) every 1.4 days. The planet candidate is roughly the same size as Jupiter and is no more than 14 times as massive (with 95% confidence). Other cases of white dwarfs with close brown dwarf or stellar companions are explained as the consequence of common-envelope evolution, wherein the original orbit is enveloped during the red-giant phase and shrinks due to friction. In this case, though, the low mass and relatively long orbital period of the planet candidate make common-envelope evolution less likely. Instead, the WD 1856+534 system seems to demonstrate that giant planets can be scattered into tight orbits without being tidally disrupted, and motivates searches for smaller transiting planets around white dwarfs. WD 1856+534 (hereafter, WD 1856 for brevity) is located 25 parsecs away in a visual triple star system. It has an effective temperature of 4710 ± 60 Kelvin and became a white dwarf 5.9 ± 0.5 billion years ago, based on theoretical models for how white dwarfs cool over time. The total system age, including the star's main sequence lifetime, must be older. Table 1 gives the other key parameters of the star. WD 1856 is one of thousands of white dwarfs that was targeted for observations with NASA's Transiting Exoplanet Survey Satellite (TESS ), in order to search for any periodic dimming events caused by planetary transits. A statistically significant transit-like event was detected by the TESS Science Processing Operations Center (SPOC) pipeline based

show abstract

Section: Spitzer Observationsmentioning

confidence: 99%

A giant planet candidate transiting a white dwarf

Vanderburg

Rappaport

et al. 2020

Nature

Self Cite

183

101

View full text Add to dashboard Cite

show abstract

“…We constrained the visual-binary orbital parameters using the LOFTI_gaiaDR2 software package (Pearce et al 2020). LOFTI_gaiaDR2 uses the instantaneous positions, proper motions, and masses of the components of visual-binary stars to estimate their orbital parameters.…”

Section: | ( ) mentioning

confidence: 99%

Two Bright M Dwarfs Hosting Ultra-Short-Period Super-Earths with Earth-like Compositions*

Hirano

Livingston

Fukui

et al. 2021

Self Cite

View full text Add to dashboard Cite

We present observations of two bright M dwarfs (TOI-1634 and TOI-1685: J = 9.5-9.6) hosting ultra-short-period (USP) planets identified by the TESS mission. The two stars are similar in temperature, mass, and radius (T eff ≈ 3500 K, M å ≈ 0.45-0.46 M e , and R å ≈ 0.45-0.46 R e ), and the planets are both super-Earth size (1.25 R ⊕ < R p < 2.0 R ⊕ ). For both systems, light curves from ground-based photometry exhibit planetary transits, whose depths are consistent with those from the TESS photometry. We also refine the transit ephemerides based on the ground-based photometry, finding the orbital periods of P = 0.9893436 ± 0.0000020 days and P = 0.6691416 ± 0.0000019 days for TOI-1634b and TOI-1685b, respectively. Through intensive radial velocity (RV) observations using the InfraRed Doppler (IRD) instrument on the Subaru 8.2 m telescope, we confirm the planetary nature of the TOIs and measure their masses: 10.14 ± 0.95 M ⊕ and 3.43 ± 0.93 M ⊕ for TOI-1634b and TOI-1685b, respectively, when the observed RVs are fitted with a single-planet circular-orbit model. Combining those with the planet radii of R p = 1.749 ± 0.079 R ⊕ (TOI-1634b) and 1.459 ± 0.065 R ⊕ (TOI-1685b), we find that both USP planets have mean densities consistent with an Earth-like internal composition, which is typical for small USP planets. TOI-1634b is currently the most massive USP planet in this category, and it resides near the radius valley, which makes it a benchmark planet in the context of discussing the size limit of rocky planet cores as well as testing the formation scenarios for USP planets. Excess scatter in the RV residuals for TOI-1685 suggests the presence of a possible secondary planet or unknown activity/instrumental noise in the RV data, but further observations are required to check those possibilities.

show abstract

“…Article number, page 10 of 25 Figures 10 and 11 show the comparison between the 95% and the 68 % gas-to-dust disc size ratios measured in our sample of multiple stellar systems in the Taurus region, and the one measured by Sanchis et al (2021) for 42 discs in the Lupus starforming regions, which are mainly singles or, in two cases, in wide binary systems with separation ∼ 1000 au, high enough that discs are not affected by tidal truncation (Pearce et al 2020).…”

Section: Comparing Dust and Gas Disc Radiimentioning

confidence: 96%

“…GK Tau and GI Tau are possibly part of a bound system. However, considering the high separation of the targets (∼ 1700 au; Hartigan et al 1994, Herczeg & Hillenbrand 2014) the sizes of both GI Tau and GK Tau are not affected by tidal truncation (Pearce et al 2020), and are thus excluded from the analysis in this work. Finally, the observation of UY Aur and T Tau do not show a velocity pattern compatible with Keplerian rotation (see Section 3), making it difficult to determine if the gas emission is reflecting the disc dynamics, and therefore to estimate the radius of individual discs.…”

Section: Sample Propertiesmentioning

confidence: 99%

Observational constraints on disc sizes in protoplanetary discs in multiple systems in the Taurus region. II. Gas disc sizes

Rota,

Manara,

Miotello

et al. 2022

Preprint

View full text Add to dashboard Cite

The formation of multiple stellar systems is a natural by-product of the star-formation process, and its impact on the properties of protoplanetary discs and on the formation of planets is still to be fully understood. To date, no detailed uniform study of the gas emission from a sample of protoplanetary discs around multiple stellar systems has been performed. Here we analyse new ALMA observations at a ∼21 au resolution of the molecular CO gas emission targeting discs in eight multiple stellar systems in the Taurus star-forming regions. 12 CO gas emission is detected around all primaries and in seven companions. With these data, we estimate the inclination and the position angle for all primary discs and for five secondary or tertiary discs, and measure the gas disc radii of these objects with a cumulative flux technique on the spatially resolved zeroth moment images. When considering the radius including 95% of the flux as a metric, the estimated gas disc size in multiple stellar systems is found to be on average ∼ 4.2 times larger than the dust disc size. This ratio is higher than what was recently found in a population of more isolated and single systems. On the contrary, when considering the radius including 68% of the flux, no difference between multiple and single discs is found in the distribution of ratios. This discrepancy is due to the sharp truncation of the outer dusty disc observed in multiple stellar systems. The measured gas disc sizes are consistent with tidal truncation models in multiple stellar systems assuming eccentricities of ∼ 0.15-0.5, as expected in typical binary systems.

show abstract

Orbital Parameter Determination for Wide Stellar Binary Systems in the Age of Gaia

Cited by 44 publications

References 86 publications

A giant planet candidate transiting a white dwarf

A giant planet candidate transiting a white dwarf

Two Bright M Dwarfs Hosting Ultra-Short-Period Super-Earths with Earth-like Compositions*

Observational constraints on disc sizes in protoplanetary discs in multiple systems in the Taurus region. II. Gas disc sizes

Contact Info

Product

Resources

About