A Short-Period Censor of Sub-Jupiter Mass Exoplanets With Low Density

Szabó, Gy. M.; Kiss, L. L.

doi:10.1088/2041-8205/727/2/l44

Cited by 177 publications

(134 citation statements)

References 26 publications

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“…Following Szabó & Kiss (2011), we study here the location and shape of the desert in both the period-mass and period-radius planes using the large accumulating samples of planets available today. For the period-mass plane we use the set of detected planets with derived masses that appear in the exoplanet encyclopedia 1 .…”

Section: Introductionmentioning

confidence: 99%

Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes

Mazeh

Holczer

Faigler

2016

A&A

289

351

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A few studies have reported a significant dearth of exoplanets with Neptune mass and radius with orbital periods below 2-4 d. This cannot be explained by observational biases because many Neptunian planets with longer orbital periods have been detected. The existence of this desert is similar to the appearance of the so-called brown-dwarf desert that suggests different formation mechanisms of planets and stellar companions with short orbital periods. Similarly, the Neptunian desert might indicate different mechanisms of formation and evolution for hot Jupiters and short-period super-Earths. We here follow a previous study and examine the location and shape of the desert in both the period-mass and period-radius planes, using the currently available large samples of planets. The desert in the period-mass plane has a relatively sharp upper edge, with a planetary mass that is inversely proportional to the planetary orbital period, while the lower, somewhat blurred, boundary is located along masses that are apparently linearly proportional to the period. The desert in the period-radius plane of the transiting planets is less clear. It seems as if the radius along the upper boundary is inversely proportional to the period to the power of one-third, while the lower boundary shows a radius that is proportional to the period to the power of two-thirds. The combination of the two upper bounds of the desert, in the period-mass and period-radius planes, yields a planetary mass-radius relation of R p /R Jup (1.2 ± 0.3)(M p /M Jup ) 0.27 ± 0.11 for 0.1 M p /M Jup 1. The derived shape of the desert, which might extend up to periods of 5-10 d, could shed some light on the formation and evolution of close-in planets.

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Section: Introductionmentioning

confidence: 99%

Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes

Mazeh

Holczer

Faigler

2016

A&A

289

351

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“…The size of KOI-13.01 is 2.2±0.1 RJ . There is no example for such large planets among the known exoplanets (Szabó and Kiss, 2011). Thus, we conclude that KOI-13.01 is likely a brown dwarf, or at the very low-end of the red dwarf stars.…”

Section: Discussionmentioning

confidence: 73%

Asymmetric Transit Curves as Indication of Orbital Obliquity: Clues from the Brown Dwarf Companion in KOI-13

et al. 2011

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Abstract. Exoplanets orbiting rapidly rotating stars may have unusual light curve shapes. These objects transit across an oblate disk with non-isotropic surface brightness, caused by the gravitational darkening. If such asymmetries are measured, one can infer the orbital obliquity of the exoplanet and the gravity darkened star, even without the analysis of the RossiterMcLaughlin effect or interferometry. Here we introduce KOI-13 as the first example of a transiting system with a gravity darkened star.

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“…Patterns in the demographics of short period planets [45][46][47][48] are due to a significant lack of short period planets at intermediate mass or radius: the Neptunian desert 49 . This feature cannot be due to observational selection effects and has persisted as more exoplanets have been discovered.…”

Section: Dmpp Circumstellar Gas and Exoplanet Demographicsmentioning

confidence: 99%

Dispersed Matter Planet Project discoveries of ablating planets orbiting nearby bright stars

et al. 2019

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Some highly irradiated close-in exoplanets orbit stars showing anomalously low stellar chromospheric emission. We attribute this to absorption by circumstellar gas replenished by mass loss from ablating planets. Here we report statistics validating this hypothesis. Among ~3000 nearby, bright, main sequence stars ~40 show depressed 51chromospheric emission indicative of undiscovered mass-losing planets. The Dispersed Matter Planet Project uses high precision, high cadence radial velocity measurements to detect these planets. We summarise results for two planetary systems (DMPP-1 and DMPP-3) and fully present observations revealing a Mp sin i = 0.469 MJ planet in a 5.207 d orbit around the γ-Doradus pulsator HD 11231 (DMPP-2). We have detected short period planets wherever we have made more than 60 RV measurements, demonstrating that we have originated a very efficient method for detecting nearby compact planetary systems. Our shrouded, ablating planetary systems may be a shortlived phase related to the Neptunian desert: i.e. the dearth of intermediate-mass planets at short orbital periods. The circumstellar gas facilitates compositional analysis; allowing empirical exogeology in the cases of sublimating rocky planets. Dispersed Matter Planet Project discoveries will be important for establishing the empirical mass-radius-composition relationship(s) for low mass planets.Massive planets in short period orbits were the first exoplanets to be discovered, but their low-mass analogues remained elusive for almost two decades. Recently, however, Kepler results have established there is a significant population of low-mass, ultra-short period (USP) planets: 0.51 ± 0.07% of G dwarfs host low-mass USP planets with Porb < 1 d 1 . Most of these planets are smaller than 2 R⊕. Kepler has a narrow field of view, so the planets it discovers are generally distant and difficult to study in detail. Radial velocity (RV) mass determinations of the overwhelming majority of Kepler's small planet discoveries are consequently more-or-less precluded. Nearby analogues of these Kepler USPs must exist, but an enormous effort would be required to find them through targeted RV observations of bright nearby stars with only a 0.5% chance of success for each target. DMPP selects target stars likely to host planets with short orbital periods using archival stellar spectral information. This paper (i) explains the motivation and underlying hypothesis for the DMPP selection criteria, which were developed using inferences from observations of transiting hot Jupiters; (ii) uses the statistics of our first three DMPP planetary system discoveries to test the underlying hypothesis (iii) presents the discovery of DMPP-2 and our RV survey methodology. Companion papers present the discoveries of DMPP-1 and DMPP-3 (this issue of NA); the characteristics of these two systems are briefly summarised to place the hypothesis testing in context.The discovery of an extensive H I exosphere surrounding the hot Jupiter HD 209458 b 2 , and subsequent evidence suggests th...

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A Short-Period Censor of Sub-Jupiter Mass Exoplanets With Low Density

Cited by 177 publications

References 26 publications

Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes

Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes

Asymmetric Transit Curves as Indication of Orbital Obliquity: Clues from the Brown Dwarf Companion in KOI-13

Dispersed Matter Planet Project discoveries of ablating planets orbiting nearby bright stars

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