University of Hertfordshire

From the same journal

By the same authors

AD Leonis: Radial velocity signal of stellar rotation or spin-orbit resonance?

Research output: Contribution to journalArticlepeer-review

Standard

AD Leonis : Radial velocity signal of stellar rotation or spin-orbit resonance? / Tuomi, Mikko; Jones, Hugh R. A.; Anglada-Escudé, Guillem; Butler, R. Paul; Kiraga, Marcin; Vogt, Steven S.

In: The Astronomical Journal, Vol. 155, No. 5, 192, 16.04.2018, p. 192.

Research output: Contribution to journalArticlepeer-review

Harvard

Tuomi, M, Jones, HRA, Anglada-Escudé, G, Butler, RP, Kiraga, M & Vogt, SS 2018, 'AD Leonis: Radial velocity signal of stellar rotation or spin-orbit resonance?', The Astronomical Journal, vol. 155, no. 5, 192, pp. 192. https://doi.org/10.3847/1538-3881/aab09c

APA

Vancouver

Author

Tuomi, Mikko ; Jones, Hugh R. A. ; Anglada-Escudé, Guillem ; Butler, R. Paul ; Kiraga, Marcin ; Vogt, Steven S. / AD Leonis : Radial velocity signal of stellar rotation or spin-orbit resonance?. In: The Astronomical Journal. 2018 ; Vol. 155, No. 5. pp. 192.

Bibtex

@article{22357e968fe84c309a1357c438679c0d,
title = "AD Leonis: Radial velocity signal of stellar rotation or spin-orbit resonance?",
abstract = "AD Leonis is a nearby magnetically active M dwarf. We find Doppler variability with a period of 2.23 days, as well as photometric signals: (1) a short-period signal, which is similar to the radial velocity signal, albeit with considerable variability; and (2) a long-term activity cycle of 4070 ± 120 days. We examine the short-term photometric signal in the available All-Sky Automated Survey and Microvariability and Oscillations of STars (MOST) photometry and find that the signal is not consistently present and varies considerably as a function of time. This signal undergoes a phase change of roughly 0.8 rad when considering the first and second halves of the MOST data set, which are separated in median time by 3.38 days. In contrast, the Doppler signal is stable in the combined High-Accuracy Radial velocity Planet Searcher and High Resolution Echelle Spectrometer radial velocities for over 4700 days and does not appear to vary in time in amplitude, phase, period, or as a function of extracted wavelength. We consider a variety of starspot scenarios and find it challenging to simultaneously explain the rapidly varying photometric signal and the stable radial velocity signal as being caused by starspots corotating on the stellar surface. This suggests that the origin of the Doppler periodicity might be the gravitational tug of a planet orbiting the star in spin-orbit resonance. For such a scenario and no spin-orbit misalignment, the measured indicates an inclination angle of 15.°5 ± 2.°5 and a planetary companion mass of 0.237 ± 0.047 M Jup. ",
keywords = "methods: numerical, methods: statistical, techniques: radial velocities",
author = "Mikko Tuomi and Jones, {Hugh R. A.} and Guillem Anglada-Escud{\'e} and Butler, {R. Paul} and Marcin Kiraga and Vogt, {Steven S.}",
note = "This is an Open Access article. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.",
year = "2018",
month = apr,
day = "16",
doi = "10.3847/1538-3881/aab09c",
language = "English",
volume = "155",
pages = "192",
journal = "The Astronomical Journal ",
issn = "0004-6256",
publisher = "IOP Publishing Ltd.",
number = "5",

}

RIS

TY - JOUR

T1 - AD Leonis

T2 - Radial velocity signal of stellar rotation or spin-orbit resonance?

AU - Tuomi, Mikko

AU - Jones, Hugh R. A.

AU - Anglada-Escudé, Guillem

AU - Butler, R. Paul

AU - Kiraga, Marcin

AU - Vogt, Steven S.

N1 - This is an Open Access article. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.

PY - 2018/4/16

Y1 - 2018/4/16

N2 - AD Leonis is a nearby magnetically active M dwarf. We find Doppler variability with a period of 2.23 days, as well as photometric signals: (1) a short-period signal, which is similar to the radial velocity signal, albeit with considerable variability; and (2) a long-term activity cycle of 4070 ± 120 days. We examine the short-term photometric signal in the available All-Sky Automated Survey and Microvariability and Oscillations of STars (MOST) photometry and find that the signal is not consistently present and varies considerably as a function of time. This signal undergoes a phase change of roughly 0.8 rad when considering the first and second halves of the MOST data set, which are separated in median time by 3.38 days. In contrast, the Doppler signal is stable in the combined High-Accuracy Radial velocity Planet Searcher and High Resolution Echelle Spectrometer radial velocities for over 4700 days and does not appear to vary in time in amplitude, phase, period, or as a function of extracted wavelength. We consider a variety of starspot scenarios and find it challenging to simultaneously explain the rapidly varying photometric signal and the stable radial velocity signal as being caused by starspots corotating on the stellar surface. This suggests that the origin of the Doppler periodicity might be the gravitational tug of a planet orbiting the star in spin-orbit resonance. For such a scenario and no spin-orbit misalignment, the measured indicates an inclination angle of 15.°5 ± 2.°5 and a planetary companion mass of 0.237 ± 0.047 M Jup.

AB - AD Leonis is a nearby magnetically active M dwarf. We find Doppler variability with a period of 2.23 days, as well as photometric signals: (1) a short-period signal, which is similar to the radial velocity signal, albeit with considerable variability; and (2) a long-term activity cycle of 4070 ± 120 days. We examine the short-term photometric signal in the available All-Sky Automated Survey and Microvariability and Oscillations of STars (MOST) photometry and find that the signal is not consistently present and varies considerably as a function of time. This signal undergoes a phase change of roughly 0.8 rad when considering the first and second halves of the MOST data set, which are separated in median time by 3.38 days. In contrast, the Doppler signal is stable in the combined High-Accuracy Radial velocity Planet Searcher and High Resolution Echelle Spectrometer radial velocities for over 4700 days and does not appear to vary in time in amplitude, phase, period, or as a function of extracted wavelength. We consider a variety of starspot scenarios and find it challenging to simultaneously explain the rapidly varying photometric signal and the stable radial velocity signal as being caused by starspots corotating on the stellar surface. This suggests that the origin of the Doppler periodicity might be the gravitational tug of a planet orbiting the star in spin-orbit resonance. For such a scenario and no spin-orbit misalignment, the measured indicates an inclination angle of 15.°5 ± 2.°5 and a planetary companion mass of 0.237 ± 0.047 M Jup.

KW - methods: numerical

KW - methods: statistical

KW - techniques: radial velocities

UR - http://www.scopus.com/inward/record.url?scp=85047347851&partnerID=8YFLogxK

U2 - 10.3847/1538-3881/aab09c

DO - 10.3847/1538-3881/aab09c

M3 - Article

VL - 155

SP - 192

JO - The Astronomical Journal

JF - The Astronomical Journal

SN - 0004-6256

IS - 5

M1 - 192

ER -