The Inner 25 au Debris Distribution in the ϵ Eri System

Su, K. Y. L.; Buizer, James M. De; Rieke, G. H.; Krivov, A. V.; Löhne, T.; Marengo, Massimo; Stapelfeldt, K.; Ballering, Nicholas P.; Vacca, William D.

doi:10.3847/1538-3881/aa696b

Cited by 53 publications

(44 citation statements)

References 57 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Eridani (Schütz et al 2004;Backman et al 2009;Greaves et al 2014;Lestrade & Thilliez 2015;MacGregor et al 2015;Su et al 2017) and HR 8799 (Marois et al 2008;Rhee et al 2007;Su et al 2009;Marois et al 2010;Matthews et al 2014;Contro et al 2016) are two such examples, both having multiple asteroid belts and hosting (or are proposed to host) several giant planets, just as we find in the Solar system. However, none have thus far been found to host rocky planets in their HZs.…”

Section: Searching For Solar System Analoguesmentioning

confidence: 64%

Properties of the single Jovian planet population and the pursuit of Solar system analogues

Agnew

Maddison

Horner

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

While the number of exoplanets discovered continues to increase at a rapid rate, we are still to discover any system that truly resembles the Solar system. Existing and near future surveys will likely continue this trend of rapid discovery. To see if these systems are Solar system analogues, we will need to efficiently allocate resources to carry out intensive follow-up observations. We seek to uncover the properties and trends across systems that indicate how much of the habitable zone is stable in each system to provide focus for planet hunters. We study the dynamics of all known single Jovian planetary systems, to assess the dynamical stability of the habitable zone around their host stars. We perform a suite of simulations of all systems where the Jovian planet will interact gravitationally with the habitable zone, and broadly classify these systems.Besides the system's mass ratio (M pl /M st ar ), and the Jovian planet's semi-major axis (a pl ) and eccentricity (e pl ), we find that there are no underlying system properties which are observable that indicate the potential for planets to survive within the system's habitable zone. We use M pl /M st ar , a pl and e pl to generate a parameter space over which the unstable systems cluster, thus allowing us to predict which systems to exclude from future observational or numerical searches for habitable exoplanets. We also provide a candidate list of 20 systems that have completely stable habitable zones and Jovian planets orbiting beyond the habitable zone as potential first order Solar system analogues.

show abstract

Section: Searching For Solar System Analoguesmentioning

confidence: 64%

Properties of the single Jovian planet population and the pursuit of Solar system analogues

Agnew

Maddison

Horner

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…The detection of dust interior to the main ring in the mm calls into question the Reidemeister et al (2011) model as they show that the drag forces only have a strong effect on grains with sizes 10 µm that are expected to be very faint at long wavelengths. Su et al (2017) show that the (Reidemeister et al 2011) model is inconsistent with observations from the Stratospheric Observatory for Infrared Astronomy (SOFIA), whilst the models of Backman et al (2009) and Greaves et al (2014b) are consistent with them.…”

Section: Introductionmentioning

confidence: 82%

The Northern arc of ε Eridani’s Debris Ring as seen by ALMA

Booth

Dent

Jordán

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present the first ALMA observations of the closest known extrasolar debris disc. This disc orbits the star Eri, a K-type star just 3.2 pc away. Due to the proximity of the star, the entire disc cannot fit within the ALMA field of view. Therefore, the observations have been centred 18 North of the star, providing us with a clear detection of the northern arc of the ring, at a wavelength of 1.3 mm. The observed disc emission is found to be narrow with a width of just 11-13 AU. The fractional disc width we find is comparable to that of the Solar System's Kuiper Belt and makes this one of the narrowest debris discs known. If the inner and outer edges are due to resonances with a planet then this planet likely has a semi-major axis of 48 AU. We find tentative evidence for clumps in the ring, although there is a strong chance that at least one is a background galaxy. We confirm, at much higher significance, the previous detection of an unresolved emission at the star that is above the level of the photosphere and attribute this excess to stellar chromospheric emission.

show abstract

“…, which suggests a contribution from background contamination. Excess emission interior to the wellknown ring has been detected by a combination of direct imaging, mIR spectroscopy, and spectral energy distribution (SED) modeling (Backman et al 2009;Reidemeister et al 2011;Greaves et al 2014) and was resolved with a size of ∼12 AU (Su et al 2017). Additional mm-wave emission at the location of the star is likely due to stellar chromospheric emission (MacGregor et al 2015;Booth et al 2017).…”

Section: )mentioning

confidence: 99%

The HOSTS Survey—Exozodiacal Dust Measurements for 30 Stars

Ertel

Defrère

Hinz

et al. 2018

Self Cite

View full text Add to dashboard Cite

The HOSTS (Hunt for Observable Signatures of Terrestrial Systems) survey searches for dust near the habitable zones (HZs) around nearby, bright main sequence stars. We use nulling interferometry in N band to suppress the bright stellar light and to probe for low levels of HZ dust around the 30 stars observed so far. Our overall detection rate is 18%, including four new detections, among which are the first three around Sun-like stars and the first two around stars without any previously known circumstellar dust. The inferred occurrence rates are comparable for early type and Sun-like stars, but decrease from 60 +16 −21 % for stars with previously detected cold dust to 8 +10 −3 % for stars without such excess, confirming earlier results at higher sensitivity. For completed observations on individual stars, our sensitivity is five to ten times better than previous results. Assuming a lognormal excess luminosity function, we put upper limits on the median HZ dust level of 13 zodis (95% confidence) for a sample of stars without cold dust and of 26 zodis when focussing on Sun-like stars without cold dust. However, our data suggest that a more complex luminosity function may be more appropriate. For stars without detectable LBTI excess, our upper limits are almost reduced by a factor of two, demonstrating the strength of LBTI target vetting for future exo-Earth imaging missions. Our statistics are so far limited and extending the survey is critical to inform the design of future exo-Earth imaging surveys.

show abstract

The Inner 25 au Debris Distribution in the ϵ Eri System

Cited by 53 publications

References 57 publications

Properties of the single Jovian planet population and the pursuit of Solar system analogues

Properties of the single Jovian planet population and the pursuit of Solar system analogues

The Northern arc of ε Eridani’s Debris Ring as seen by ALMA

The HOSTS Survey—Exozodiacal Dust Measurements for 30 Stars

Contact Info

Product

Resources

About