ORCID Profile
0000-0001-6285-267X
Current Organisations
University of Washington
,
University of Colorado
,
Goddard Space Flight Center
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Publisher: Springer Science and Business Media LLC
Date: 10-2023
Publisher: American Astronomical Society
Date: 21-10-2015
Publisher: American Astronomical Society
Date: 05-2022
Publisher: American Astronomical Society
Date: 27-06-2019
Publisher: American Geophysical Union (AGU)
Date: 02-2021
DOI: 10.1029/2020JE006643
Abstract: Over the past several decades, thousands of planets have been discovered outside our Solar System. These planets exhibit enormous ersity, and their large numbers provide a statistical opportunity to place our Solar System within the broader context of planetary structure, atmospheres, architectures, formation, and evolution. Meanwhile, the field of exoplanetary science is rapidly forging onward toward a goal of atmospheric characterization, inferring surface conditions and interiors, and assessing the potential for habitability. However, the interpretation of exoplanet data requires the development and validation of exoplanet models that depend on in situ data that, in the foreseeable future, are only obtainable from our Solar System. Thus, planetary and exoplanetary science would both greatly benefit from a symbiotic relationship with a two‐way flow of information. Here, we describe the critical lessons and outstanding questions from planetary science, the study of which are essential for addressing fundamental aspects for a variety of exoplanetary topics. We outline these lessons and questions for the major categories of Solar System bodies, including the terrestrial planets, the giant planets, moons, and minor bodies. We provide a discussion of how many of these planetary science issues may be translated into exoplanet observables that will yield critical insight into current and future exoplanet discoveries.
Publisher: American Astronomical Society
Date: 19-04-2016
Publisher: American Astronomical Society
Date: 02-2021
Abstract: The observation of a 266.94 GHz feature in the Venus spectrum has been attributed to phosphine (PH 3 ) in the Venus clouds, suggesting unexpected geological, chemical, or even biological processes. Since both PH 3 and sulfur dioxide (SO 2 ) are spectrally active near 266.94 GHz, the contribution to this line from SO 2 must be determined before it can be attributed, in whole or part, to PH 3 . An undetected SO 2 reference line, interpreted as an unexpectedly low SO 2 abundance, suggested that the 266.94 GHz feature could be attributed primarily to PH 3 . However, the low SO 2 and the inference that PH 3 was in the cloud deck posed an apparent contradiction. Here we use a radiative transfer model to analyze the PH 3 discovery, and explore the detectability of different vertical distributions of PH 3 and SO 2 . We find that the 266.94 GHz line does not originate in the clouds, but above 80 km in the Venus mesosphere. This level of line formation is inconsistent with chemical modeling that assumes generation of PH 3 in the Venus clouds. Given the extremely short chemical lifetime of PH 3 in the Venus mesosphere, an implausibly high source flux would be needed to maintain the observed value of 20 ± 10 ppb. We find that typical Venus SO 2 vertical distributions and abundances fit the JCMT 266.94 GHz feature, and the resulting SO 2 reference line at 267.54 GHz would have remained undetectable in the ALMA data due to line dilution. We conclude that nominal mesospheric SO 2 is a more plausible explanation for the JCMT and ALMA data than PH 3 .
Publisher: Springer Science and Business Media LLC
Date: 16-07-2021
Publisher: Springer Science and Business Media LLC
Date: 31-10-2023
Publisher: American Astronomical Society
Date: 02-2023
Abstract: We report the discovery of TOI-700 e, a 0.95 R ⊕ planet residing in the Optimistic Habitable Zone (HZ) of its host star. This discovery was enabled by multiple years of monitoring from NASA’s Transiting Exoplanet Survey Satellite (TESS) mission. The host star, TOI-700 (TIC 150428135), is a nearby (31.1 pc), inactive, M2.5 dwarf ( V mag = 13.15). TOI-700 is already known to host three planets, including the small, HZ planet, TOI-700 d. The new planet has an orbital period of 27.8 days, and based on its radius (0.95 R ⊕ ), it is likely rocky. TOI-700 was observed for 21 sectors over Years 1 and 3 of the TESS mission, including 10 sectors at 20 s cadence in Year 3. Using this full set of TESS data and additional follow-up observations, we identify, validate, and characterize TOI-700 e. This discovery adds another world to the short list of small, HZ planets transiting nearby and bright host stars. Such systems, where the stars are bright enough that follow-up observations are possible to constrain planet masses and atmospheres using current and future facilities, are incredibly valuable. The presence of multiple small, HZ planets makes this system even more enticing for follow-up observations.
Publisher: American Astronomical Society
Date: 11-2018
Publisher: American Astronomical Society
Date: 08-02-2017
No related grants have been discovered for Giada Arney.