Detecting Exoplanets Using Eclipsing Binaries as Natural Starshades
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Detecting Exoplanets Using Eclipsing Binaries as Natural Starshades. / Bellotti, Stefano; Zabludoff, Ann I.; Belikov, Ruslan; Guyon, Olivier; Rathi, Chirag.
I: Astronomical Journal, Bind 160, Nr. 3, 131, 25.08.2020.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Detecting Exoplanets Using Eclipsing Binaries as Natural Starshades
AU - Bellotti, Stefano
AU - Zabludoff, Ann I.
AU - Belikov, Ruslan
AU - Guyon, Olivier
AU - Rathi, Chirag
PY - 2020/8/25
Y1 - 2020/8/25
N2 - We investigate directly imaging exoplanets around eclipsing binaries using the eclipse as a natural tool for dimming the binary and thus increasing the planet to star brightness contrast. At eclipse, the binary becomes pointlike, making coronagraphy possible. We select binaries where the planet-star contrast would be boosted by >10x during eclipse, making it possible to detect a planet that is greater than or similar to 10x fainter or in a star system that is similar to 2-3x more massive than otherwise. Our approach will yield insights into planet occurrence rates around binaries versus individual stars. We consider both self-luminous (SL) and reflected light (RL) planets. In the SL case, we select binaries whose age is young enough so that an orbiting SL planet would remain luminous; in U Cep and AC Sct, respectively, our method is sensitive to SL planets of similar to 4.5 and similar to 9M(J)with current ground- or near-future space-based instruments and similar to 1.5 and similar to 6M(J)with future ground-based observatories. In the RL case, there are three nearby (less than or similar to 50 pc) systems-V1412 Aql, RR Cae, and RT Pic-around which a Jupiter-like planet at a planet-star separation of greater than or similar to 20 mas might be imaged with future ground- and space-based coronagraphs. A Venus-like planet at the same distance might be detectable around RR Cae and RT Pic. A habitable Earth-like planet represents a challenge; while the planet-star contrast at eclipse and planet flux are accessible with a 6-8 m space telescope, the planet-star separation is 1/3-1/4 of the angular separation limit of modern coronagraphy.
AB - We investigate directly imaging exoplanets around eclipsing binaries using the eclipse as a natural tool for dimming the binary and thus increasing the planet to star brightness contrast. At eclipse, the binary becomes pointlike, making coronagraphy possible. We select binaries where the planet-star contrast would be boosted by >10x during eclipse, making it possible to detect a planet that is greater than or similar to 10x fainter or in a star system that is similar to 2-3x more massive than otherwise. Our approach will yield insights into planet occurrence rates around binaries versus individual stars. We consider both self-luminous (SL) and reflected light (RL) planets. In the SL case, we select binaries whose age is young enough so that an orbiting SL planet would remain luminous; in U Cep and AC Sct, respectively, our method is sensitive to SL planets of similar to 4.5 and similar to 9M(J)with current ground- or near-future space-based instruments and similar to 1.5 and similar to 6M(J)with future ground-based observatories. In the RL case, there are three nearby (less than or similar to 50 pc) systems-V1412 Aql, RR Cae, and RT Pic-around which a Jupiter-like planet at a planet-star separation of greater than or similar to 20 mas might be imaged with future ground- and space-based coronagraphs. A Venus-like planet at the same distance might be detectable around RR Cae and RT Pic. A habitable Earth-like planet represents a challenge; while the planet-star contrast at eclipse and planet flux are accessible with a 6-8 m space telescope, the planet-star separation is 1/3-1/4 of the angular separation limit of modern coronagraphy.
KW - Eclipsing binary stars
KW - Exoplanets
KW - Direct imaging
KW - Coronagraphic imaging
KW - CIRCUMBINARY PLANETS
KW - CATALOG
KW - SPECTROSCOPY
KW - DWARFS
KW - SYSTEM
KW - IMAGES
KW - DISK
KW - NAOS
KW - 1ST
U2 - 10.3847/1538-3881/aba7c6
DO - 10.3847/1538-3881/aba7c6
M3 - Journal article
VL - 160
JO - The Astronomical Journal
JF - The Astronomical Journal
SN - 0004-6256
IS - 3
M1 - 131
ER -
ID: 248600288