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29 March 2024 |
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Testing the Spectroscopic Extraction of Suppression of Convective Blueshift | M. Miklos
; T. W. Milbourne
; R. D. Haywood
; D. F. Phillips
; S. H. Saar
; N. Meunier
; H. M. Cegla
; X. Dumusque
; N. Langellier
; J. Maldonado
; L. Malavolta
; A. Mortier
; S. Thompson
; C. A. Watson
; M. Cecconi
; R. Cosentino
; A. Ghedina
; C-H. Li
; M. López-Morales
; E. Molinari
; E. Poretti
; D. Sasselov
; A. Sozzetti
; R. L. Walsworth
; | Date: |
20 Oct 2019 | Abstract: | Efforts to detect low-mass exoplanets using stellar radial velocities (RVs)
are currently limited by magnetic photospheric activity. Suppression of
convective blueshift is the dominant magnetic contribution to RV variability in
low-activity Sun-like stars. Due to plasma motion driven by convective
processes, the magnitude of RV contributions from the suppression of convective
blueshift is proportional to the depth of formation of photospheric spectral
lines used to compute the RV time series. Meunier et al. 2017 used this
relation to demonstrate a method for spectroscopic extraction of the
suppression of convective blueshift in order to isolate RV contributions,
including planetary RVs, that contribute equally to the timeseries for each
spectral line. Here, we extract disk-integrated solar RVs from observations
over a 2.5 year time span made with the solar telescope integrated with the
HARPS-N spectrograph at the Telescopio Nazionale Galileo (La Palma, Canary
Islands, Spain). We apply the methods outlined by Meunier et al. 2017. We are
not, however, able to isolate physically meaningful contributions of the
suppression of convective blueshift from this solar dataset, potentially
because our dataset is from solar minimum when the suppression of convective
blueshift may not sufficiently dominate activity contributions to RVs. This
result indicates that, for low-activity Sun-like stars, one must include
additional RV contributions from activity sources not considered in the Meunier
et al. 2017 model at different timescales as well as instrumental variation in
order to reach the sub-meter per second RV sensitivity necessary to detect
low-mass planets in orbit around Sun-like stars. | Source: | arXiv, 1910.9038 | Services: | Forum | Review | PDF | Favorites |
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