ORCID Profile
0000-0002-6243-5697
Current Organisation
Istituto nazionale di astrofisica
Does something not look right? The information on this page has been harvested from data sources that may not be up to date. We continue to work with information providers to improve coverage and quality. To report an issue, use the Feedback Form.
Publisher: SPIE
Date: 13-12-2020
DOI: 10.1117/12.2561930
Publisher: SPIE
Date: 13-12-2020
DOI: 10.1117/12.2561534
Publisher: American Astronomical Society
Date: 31-03-2020
Publisher: SPIE
Date: 27-07-2016
DOI: 10.1117/12.2232792
Publisher: American Astronomical Society
Date: 17-04-2018
Publisher: SPIE-Intl Soc Optical Eng
Date: 06-09-2022
Publisher: SPIE
Date: 17-08-2016
DOI: 10.1117/12.2234131
Publisher: American Astronomical Society
Date: 15-03-2021
Abstract: The young (50–400 Myr) A3V star β Leo is a primary target to study the formation history and evolution of extrasolar planetary systems as one of the few stars with known hot (∼1600 K), warm (∼600 K), and cold (∼120 K) dust belt components. In this paper, we present deep mid-infrared measurements of the warm dust brightness obtained with the Large Binocular Telescope Interferometer (LBTI) as part of its exozodiacal dust survey (HOSTS). The measured excess is 0.47% ± 0.050% within the central 1.5 au, rising to 0.81% ± 0.026% within 4.5 au, outside the habitable zone of β Leo. This dust level is 50 ± 10 times greater than in the solar system’s zodiacal cloud. Poynting–Robertson drag on the cold dust detected by Spitzer, and Herschel underpredicts the dust present in the habitable zone of β Leo, suggesting an additional delivery mechanism (e.g., comets) or an additional belt at ∼5.5 au. A model of these dust components is provided that implies the absence of planets more than a few Saturn masses between ∼5 au and the outer belt at ∼40 au. We also observationally constrain giant planets with the LBTI imaging channel at 3.8 μ m wavelength. Assuming an age of 50 Myr, any planet in the system between approximately 5–50 au must be less than a few Jupiter masses, consistent with our dust model. Taken together, these observations showcase the deep contrasts and detection capabilities attainable by the LBTI for both warm exozodiacal dust and giant exoplanets in or near the habitable zone of nearby stars.
Publisher: SPIE
Date: 24-07-2018
DOI: 10.1117/12.2313685
Publisher: SPIE
Date: 13-12-2020
DOI: 10.1117/12.2561849
Publisher: SPIE
Date: 30-08-2022
DOI: 10.1117/12.2630017
Publisher: SPIE
Date: 11-06-2021
DOI: 10.1117/12.2599233
Publisher: SPIE
Date: 29-08-2022
DOI: 10.1117/12.2629266
Publisher: SPIE
Date: 30-08-2022
DOI: 10.1117/12.2627640
Publisher: SPIE
Date: 30-08-2022
DOI: 10.1117/12.2629001
Publisher: SPIE
Date: 30-08-2022
DOI: 10.1117/12.2629441
Publisher: SPIE
Date: 30-08-2022
DOI: 10.1117/12.2629363
Publisher: SPIE
Date: 13-12-2020
DOI: 10.1117/12.2561251
Publisher: SPIE
Date: 13-12-2020
DOI: 10.1117/12.2561041
Publisher: American Astronomical Society
Date: 14-06-2016
Publisher: SPIE
Date: 16-06-2016
DOI: 10.1117/12.2248393
Publisher: SPIE
Date: 04-08-2016
DOI: 10.1117/12.2233795
Publisher: SPIE
Date: 27-07-2016
DOI: 10.1117/12.2233545
No related grants have been discovered for Enrico Pinna.