A super-Earth-sized planet orbiting in or near the habitable zone around Sun-like star

Thomas Barclay; Christopher J. Burke; Steve B. Howell; Jason F. Rowe; Daniel Huber; Howard Isaacson; Jon M. Jenkins; Rea Kolbl; Geoffrey W. Marcy; Elisa V. Quintana; Martin Still; Joseph D. Twicken; Stephen T. Bryson; William J. Borucki; Douglas A. Caldwell; David Ciardi; Bruce D. Clarke; Jessie L Christiansen; Jeffrey L. Coughlin; Debra A. Fischer; Jie Li; Michael R. Haas; Roger Hunter; Jack J. Lissauer; Fergal Mullally; Anima Sabale; Shawn E. Seader; Jeffrey C. Smith; Peter Tenenbaum; AKM Kamal Uddin; Susan E. Thompson

doi:10.1088/0004-637x/768/2/101

Home/Archive/arXiv

arXiv · 1304.4941

A super-Earth-sized planet orbiting in or near the habitable zone around Sun-like star

View original source ↗Read source document ↗Export metadata ↓

Abstract

We present the discovery of a super-earth-sized planet in or near the habitable zone of a sun-like star. The host is Kepler-69, a 13.7 mag G4V-type star. We detect two periodic sets of transit signals in the three-year flux time series of Kepler-69, obtained with the Kepler spacecraft. Using the very high precision Kepler photometry, and follow-up observations, our confidence that these signals represent planetary transits is >99.1%. The inner planet, Kepler-69b, has a radius of 2.24+/-0.4 Rearth and orbits the host star every 13.7 days. The outer planet, Kepler-69c, is a super-Earth-size object with a radius of 1.7+/-0.3 Rearth and an orbital period of 242.5 days. Assuming an Earth-like Bond albedo, Kepler-69c has an equilibrium temperature of 299 +/- 19 K, which places the planet close to the habitable zone around the host star. This is the smallest planet found by Kepler to be orbiting in or near habitable zone of a Sun-like star and represents an important step on the path to finding the first true Earth analog.

Explore related subjects

astro-ph.EP

Keep this discovery

BibTeX RIS

Thomas Barclay, Christopher J. Burke, Steve B. Howell, Jason F. Rowe, Daniel Huber, Howard Isaacson, Jon M. Jenkins, Rea Kolbl, Geoffrey W. Marcy, Elisa V. Quintana, Martin Still, Joseph D. Twicken, Stephen T. Bryson, William J. Borucki, Douglas A. Caldwell, David Ciardi, Bruce D. Clarke, Jessie L Christiansen, Jeffrey L. Coughlin, Debra A. Fischer, Jie Li, Michael R. Haas, Roger Hunter, Jack J. Lissauer, Fergal Mullally, Anima Sabale, Shawn E. Seader, Jeffrey C. Smith, Peter Tenenbaum, AKM Kamal Uddin, Susan E. Thompson. 2013-04-17. A super-Earth-sized planet orbiting in or near the habitable zone around Sun-like star. https://doi.org/10.1088/0004-637x/768/2/101

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Planetary Accretion Is Less Frequent in Wide Binaries: Evidence from Metal-Enriched White Dwarfs in DESI DR1

Binary stars are common in the Galaxy, and understanding how stellar binarity influences the formation and evolution of planetary systems is an active area of research. In this study, we use metal-enriched white dwarfs in wide binaries as tracers of long-lived planetary systems. With Data Release 1 from the Dark Energy Spectroscopic Instrument (DESI), we find that the fraction of cool metal-enriched white dwarfs in wide binaries is 9.8\,$\pm$\,2.1\%, significantly lower (4.7\,$\sigma$) than the 20.5\,$\pm$\,0.9\% in a control sample of single systems. Furthermore, we identify a tentative dependence of metal enrichment on projected separation and white dwarf effective temperature, where enrichment fraction decreases at smaller separations and lower temperatures. These findings indicate that, compared to single stars, binary systems either start with smaller initial planetary reservoirs due to suppressed planetesimal formation or undergo more rapid depletion of planetary material during the initial part of the white dwarf stage.

astro-ph.EP↗

arXiv2026

The Mysterious Inspiral of WASP-12b: Why Obliquity Tides Cannot Drive Orbital Decay

WASP-12b's orbit is decaying, for unknown reasons. The planet's period is shrinking more rapidly than can be attributed to equilibrium tides or dynamical tides in a main-sequence star. Planetary obliquity tides could be sufficiently dissipative to drive WASP-12b's inspiral, but would also damp the planet's obliquity, halting the decay. Millholland & Laughlin proposed that a nearby, low-mass planet ($\sim 10$ M$_\oplus$) is maintaining a large obliquity for WASP-12b, sustaining the dissipation. We re-evaluated this hypothesis, finding that the companion must be more massive than originally proposed ($\gtrsim 65$ M$_\oplus$) to absorb WASP-12b's orbital angular momentum. Radial velocity data allowed us to rule out a companion of this type. Any companions within $3$ AU have $K \lesssim 14$ m/s at $95$% confidence.

astro-ph.EP↗

arXiv2026

Lava Tube Exploration with LunarLeaper

Lunar pits, some of which are interpreted as collapse features into underlying lava tubes, expose otherwise inaccessible stratigraphy and may provide entry points to subsurface voids that preserve records of lunar volcanism and offer potential sites for future human exploration. We synthesize the current state of knowledge on lunar pits and lava tubes, covering their morphological characteristics, classification, proposed formation mechanisms, mechanical stability, and detection from orbit. We then review the open science questions that pit and pit-wall investigation is uniquely placed to address, spanning the volcanic stratigraphy of the lunar maria, the structure and lateral variability of the regolith, and the dimensions and accessibility of subsurface conduits. To evaluate how these questions can be tackled in situ, we assess the feasibility and expected performance of geophysical and remote-sensing investigations for subsurface voids and surface exposures, mainly focusing on gravity measurements, ground-penetrating radar, high-resolution imaging, and spectroscopy. Building on this, we present LunarLeaper, a small legged robot mission concept combining a gravimeter, ground-penetrating radar, high-resolution imager, spectrometer, and leg-based geomechanical experiments to deliver the first in situ investigation of a mare pit. The concept targets the Marius Hills Pit and its associated rille, with a mobility architecture optimized for the rugged terrain encountered at pit edges and funnel slopes.

astro-ph.EP↗