The Statistics of Extended Debris Disks Measured with Gaia and Planck

Nibauer, Jacob; Baxter, Eric J.; Jain, Bhuvnesh

doi:10.3847/1538-3881/ab8192

Cited by 6 publications

(4 citation statements)

References 51 publications

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“…We have previously used a similar formalism to detect circumstellar debris disks in data from the Planck cosmic microwave background survey, constraining parameters such as the fraction of stars with debris disks (Nibauer et al 2020). The present work employs a similar modeling scheme, enabling us to place constraints on the fraction of stars with elemental depletions.…”

Section: Introductionmentioning

confidence: 99%

Statistics of the Chemical Composition of Solar Analog Stars and Links to Planet Formation

Nibauer,

Baxter,

Jain

et al. 2020

Preprint

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The Sun has been found to be depleted in refractory (rock-forming) elements relative to nearby solar analogs, suggesting a potential indicator of planet formation. Given the small amplitude of the depletion, previous analyses have primarily relied on high signal-to-noise stellar spectra and a strictly differential approach to determine elemental abundances. We present an alternative, likelihood-based approach that can be applied to much larger samples of stars with lower precision abundance determinations. We utilize measurements of about 1700 solar analogs from the Apache Point Observatory Galactic Evolution Experiment (APOGEE-2) and the stellar parameter and chemical abundance pipeline (ASPCAP DR16). By developing a hierarchical mixture model for the data, we place constraints on the statistical properties of the elemental abundances, including correlations with condensation temperature and the fraction of stars with refractory element depletions. We find evidence for two distinct populations: a depleted population of stars that makes up the majority of solar analogs including the Sun, and a not-depleted population that makes up between ∼ 10 − 30% of our sample. We find correlations with condensation temperature generally in agreement with higher precision surveys of a smaller sample of stars. Such trends, if robustly linked to the formation of planetary systems, provide a means to connect stellar chemical abundance patterns to planetary systems over large samples of Milky Way stars.

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Section: Introductionmentioning

confidence: 99%

Statistics of the Chemical Composition of Solar Analog Stars and Links to Planet Formation

Nibauer,

Baxter,

Jain

et al. 2020

Preprint

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“…Submillimeter observations using CMB surveys such as SO are well suited to characterizing disks around faint stars, such as M dwarfs, or disks at large distances from their host stars. Nibauer et al (2020) used Planck observations to place constraints on the fraction of nearby stars hosting debris disks, the majority of which were M dwarfs. The higher resolution of SO offers the potential of improved constraints: with roughly five times better angular resolution than Planck, we expect to be able to probe roughly an order of magnitude more debris disks (assuming that the measurements are confusion-limited).…”

Section: Exo-oort Clouds and Debris Disksmentioning

confidence: 99%

“…Dark and light blue regions correspond to 68% and 95% confidence regions, respectively. using a two-parameter mixture model similar to that developed in Nibauer et al (2020) and Nibauer et al (2021; in the context of debris disks and solar analog stars, respectively). Constraints on the two parametersf Oort and M Oort -are shown in the lower panel of Figure 5.…”

Section: Exo-oort Clouds and Debris Disksmentioning

confidence: 99%

The Simons Observatory: Galactic Science Goals and Forecasts

Hensley

Clark

Fanfani

et al. 2022

ApJ

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Observing in six frequency bands from 27 to 280 GHz over a large sky area, the Simons Observatory (SO) is poised to address many questions in Galactic astrophysics in addition to its principal cosmological goals. In this work, we provide quantitative forecasts on astrophysical parameters of interest for a range of Galactic science cases. We find that SO can: constrain the frequency spectrum of polarized dust emission at a level of Δβ d ≲ 0.01 and thus test models of dust composition that predict that β d in polarization differs from that measured in total intensity; measure the correlation coefficient between polarized dust and synchrotron emission with a factor of two greater precision than current constraints; exclude the nonexistence of exo-Oort clouds at roughly 2.9σ if the true fraction is similar to the detection rate of giant planets; map more than 850 molecular clouds with at least 50 independent polarization measurements at 1 pc resolution; detect or place upper limits on the polarization fractions of CO(2–1) emission and anomalous microwave emission at the 0.1% level in select regions; and measure the correlation coefficient between optical starlight polarization and microwave polarized dust emission in 1° patches for all lines of sight with N H ≳ 2 × 1020 cm−2. The goals and forecasts outlined here provide a roadmap for other microwave polarization experiments to expand their scientific scope via Milky Way astrophysics. 37 37 A supplement describing author contributions to this paper can be found at https://simonsobservatory.org/wp-content/uploads/2022/02/SO_GS_Contributions.pdf.

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“…The Oort Cloud may have evolved over the course of 100 -1000 Myr, shaped by planetary migrations, Galactic tidal forces, debris capture, and, in fact, close stellar encounters (Higuchi & Kokubo 2015;Portegies Zwart et al 2021). The Oort Cloud as we know it could be a unique structure (Portegies Zwart et al 2021), although the evolution of Oort-like structures around other stars is certainly possible over timescales of 10 -200 Myr (Portegies Zwart 2021;Portegies Zwart et al 2021), and possible microwave evidence of exo-Oort clouds around other stars has been presented (Baxter et al 2018;Nibauer et al 2020).…”

Section: Impulsementioning

confidence: 99%

Collision of Two Stellar Associations in the Nearby Gum Nebula

Yep,

White

2021

Preprint

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Based on Gaia DR2 data and new CHIRON radial velocities, we have discovered that two nearby stellar associations UPK 535 (318.08 ± 0.29 pc, 25 +15 −10 Myr, 174 stars) and Yep 3 (339.54 ± 0.25 pc , 45 +55 −20 Myr, 297 stars) in the Gum Nebula have recently collided. We project stars' current positions, motions, and measurement uncertainties backward and forward through time in a 10,000-trial Monte Carlo simulation. On average, the associations' centres of mass come within 18.89 ± 0.73 pc of each other 0.84 ± 0.03 Myr ago. A mode of 54 ± 7 close (<1 pc) stellar encounters occur during the collision. We cannot predict specific star-star close encounters with our current ∼7.6 pc distance precision and 21.5-per-cent-complete radial velocity sample. Never the less, we find that two stars in UPK 535 and two stars in Yep 3 undergo a nonspecific close encounter in >70 per cent of trials and multiple close encounters in ∼30 per cent. On average, the closest approach of any two stars is 0.13 ± 0.06 pc, or 27,000 ± 12,000 au. With impulse-tracing values up to 2.7 +3.1 −1.1 M ⊙ pc −2 km −1 s, such close encounters could perturb stars' Oort cloud comets (if present), cause heavy bombardment events for exoplanets (if present), and reshape solar system architectures. Finally, an expansion of our simulation suggests other associations in the region are also interacting. Association collisions may be commonplace, at least in the Gum Nebula straddling the Galactic plane, and may spur solar system evolution more than previously recognized.

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The Statistics of Extended Debris Disks Measured with Gaia and Planck

Cited by 6 publications

References 51 publications

Statistics of the Chemical Composition of Solar Analog Stars and Links to Planet Formation

Statistics of the Chemical Composition of Solar Analog Stars and Links to Planet Formation

The Simons Observatory: Galactic Science Goals and Forecasts

Collision of Two Stellar Associations in the Nearby Gum Nebula

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