9 research outputs found
Stable accretion and episodic outflows in the young transition disk system GM Aurigae
We investigate the structure and dynamics of the magnetospheric accretion
region and associated outflows on a scale smaller than 0.1 au around the young
transitional disk system GM Aur. We monitored the variability of the system on
timescales ranging from days to months, using high-resolution optical and
near-infrared spectroscopy, multiwavelength photometry, and low-resolution
near-infrared spectroscopy, over a total duration of six months (30 rotational
cycles). We analyzed the photometric and line profile variability to
characterize the accretion and ejection processes. The luminosity of the system
is modulated by surface spots at the stellar rotation period of 6.04 days. The
Balmer, Paschen, and Brackett hydrogen lines as well as the HeI 5876 A and HeI
10830 A line profiles are modulated on the same period. The PaB line flux
correlates with the photometric excess in the u' band, which suggests that most
of the line emission originates from the accretion process. High-velocity
redshifted absorptions reaching below the continuum periodically appear in the
near-infrared line profiles at the rotational phase in which the veiling and
line fluxes are the largest. These are signatures of a stable accretion funnel
flow and associated accretion shock at the stellar surface. This large-scale
magnetospheric accretion structure appears fairly stable over at least 15 and
possibly up to 30 rotational periods. In contrast, outflow signatures randomly
appear as blueshifted absorption components in the Balmer and HeI 10830 A line
profiles and disappear on a timescale of a few days. The coexistence of a
stable, large-scale accretion pattern and episodic outflows supports
magnetospheric ejections as the main process occurring at the star-disk
interface. Stable magnetospheric accretion and episodic outflows appear to be
physically linked on a scale of a few stellar radii in this system.Comment: 30 pages, 28 figures, 12 tables, accepted for publication in
Astronomy & Astrophysic
TOI-4860 b, a short-period giant planet transiting an M3.5 dwarf
We report the discovery and characterisation of a giant transiting planet
orbiting a nearby M3.5V dwarf (d = 80.4 pc, = 15.1 mag, =11.2 mag,
R = 0.358 0.015 R, M = 0.340 0.009
M). Using the photometric time series from TESS sectors 10, 36, 46, and
63 and near-infrared spectrophotometry from ExTrA, we measured a planetary
radius of 0.77 0.03 R and an orbital period of 1.52 days. With
high-resolution spectroscopy taken by the CFHT/SPIRou and ESO/ESPRESSO
spectrographs, we refined the host star parameters ([Fe/H] = 0.27 0.12)
and measured the mass of the planet (0.273 0.006 M). Based on these
measurements, TOI-4860 b joins the small set of massive planets (80 M)
found around mid to late M dwarfs (0.4 R), providing both an
interesting challenge to planet formation theory and a favourable target for
further atmospheric studies with transmission spectroscopy. We identified an
additional signal in the radial velocity data that we attribute to an eccentric
planet candidate () with an orbital period of ~days and
a minimum mass of M, but additional data would be needed to
confirm this.Comment: 16 pages, 14 figures, accepted for publication in A&
TOI-4860 b, a short-period giant planet transiting an M3.5 dwarf
International audienceWe report the discovery and characterisation of a giant transiting planet orbiting around a nearby M3.5V dwarf (d = 80.4 pc, G = 15.1 mag, K=11.2 mag, R = 0.354 0.011 R, M = 0.3400 0.0086 M). Using the photometric time series from the Transiting Exoplanet Survey Satellite (TESS) sectors 10, 36, 46, and 63, and near-infrared spectrophotometry from ExTrA, we measured a planetary radius of 0.766 0.026 R and an orbital period of 1.52 days. With high-resolution spectroscopy taken by the CFHT/SPIRou and ESO/ESPRESSO spectrographs, we refined the host star parameters ([Fe/H] = 0.27 0.12) and measured the mass of the planet (0.2729 0.0058 M). Based on these measurements, TOI- 4860 b joins the small set of massive planets found around mid-to-late M dwarfs (< 0.4 R), providing both an interesting challenge to planet formation theory and a favourable target for further atmospheric studies with transmission spectroscopy. We identify an additional signal in the radial velocity data that we attribute to an eccentric (e = 0.657 0.089) planet candidate with an orbital period of 426.9 7.4 days and a minimum mass of 1.66 0.26 M
TOI-4860 b, a short-period giant planet transiting an M3.5 dwarf
International audienceWe report the discovery and characterisation of a giant transiting planet orbiting around a nearby M3.5V dwarf (d = 80.4 pc, G = 15.1 mag, K=11.2 mag, R = 0.354 0.011 R, M = 0.3400 0.0086 M). Using the photometric time series from the Transiting Exoplanet Survey Satellite (TESS) sectors 10, 36, 46, and 63, and near-infrared spectrophotometry from ExTrA, we measured a planetary radius of 0.766 0.026 R and an orbital period of 1.52 days. With high-resolution spectroscopy taken by the CFHT/SPIRou and ESO/ESPRESSO spectrographs, we refined the host star parameters ([Fe/H] = 0.27 0.12) and measured the mass of the planet (0.2729 0.0058 M). Based on these measurements, TOI- 4860 b joins the small set of massive planets found around mid-to-late M dwarfs (< 0.4 R), providing both an interesting challenge to planet formation theory and a favourable target for further atmospheric studies with transmission spectroscopy. We identify an additional signal in the radial velocity data that we attribute to an eccentric (e = 0.657 0.089) planet candidate with an orbital period of 426.9 7.4 days and a minimum mass of 1.66 0.26 M
A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE and HARPS-N
We report the discovery and characterization of the transiting extrasolar
planet TOI-1710b. It was first identified as a promising candidate by the
Transiting Exoplanet Survey Satellite (TESS). Its planetary nature was then
established with SOPHIE and HARPS-N spectroscopic observations via the
radial-velocity method. The stellar parameters for the host star are derived
from the spectra and a joint Markov chain Monte-Carlo (MCMC) adjustment of the
spectral energy distribution and evolutionary tracks of TOI-1710. A joint MCMC
analysis of the TESS light curve and the radial-velocity evolution allows us to
determine the planetary system properties. From our analysis, TOI-1710b is
found to be a massive warm super-Neptune ( and ) orbiting
a G5V dwarf star () on a nearly circular
24.3-day orbit (). The orbital period of this planet is
close to the estimated rotation period of its host star and it has a low Keplerian semi-amplitude
; we thus performed additional analyses to show
the robustness of the retrieved planetary parameters. With a low bulk density
of and orbiting a bright host star (,
), TOI-1710b is one of the best targets in this mass-radius range
(near the Neptunian desert) for atmospheric characterization via transmission
spectroscopy, a key measurement in constraining planet formation and
evolutionary models of sub-Jovian planets.Comment: 18 pages, 16 figures, 5 tables, A&A in pres
A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE, and HARPS-N
We report the discovery and characterization of the transiting extrasolar planet TOI-1710 b. It was first identified as a promising candidate by the Transiting Exoplanet Survey Satellite. Its planetary nature was then established with SOPHIE and HARPS-N spectroscopic observations via the radial-velocity method. The stellar parameters for the host star are derived from the spectra and a joint Markov chain Monte-Carlo adjustment of the spectral energy distribution and evolutionary tracks of TOI-1710. A joint MCMC analysis of the TESS light curve and the radial-velocity evolution allows us to determine the planetary system properties. From our analysis, TOI-1710 b is found to be a massive warm super-Neptune (Mp = 28.3 ± 4.7 Mâ and Rp = 5.34 ± 0.11 Râ) orbiting a G5V dwarf star (Teff = 5665 ± 55 K) on a nearly circular 24.3-day orbit (e = 0.16 ± 0.08). The orbital period of this planet is close to the estimated rotation period of its host star Prot = 22.5 ± 2.0 days and it has a low Keplerian semi-amplitude K = 6.4 ± 1.0 m sâ1; we thus performed additional analyses to show the robustness of the retrieved planetary parameters. With a low bulk density of 1.03 ± 0.23 g cmâ3 and orbiting a bright host star (J = 8.3, V = 9.6), TOI-1710 b is one of the best targets in this mass-radius range (near the Neptunian desert) for atmospheric characterization via transmission spectroscopy, a key measurement in constraining planet formation and evolutionary models of sub-Jovian planets
The Breast Size Satisfaction Survey (BSSS)
The Breast Size Satisfaction Survey (BSSS) was established to assess womenâs breast size dissatisfaction and breasted experiences from a cross-national perspective. A total of 18,541 women were recruited from 61 research sites across 40 nations and completed measures of current-ideal breast size discrepancy, as well as measures of theorised antecedents (personality, Western and local media exposure, and proxies of socioeconomic status) and outcomes (weight and appearance dissatisfaction, breast awareness, and psychological well-being). In the total dataset, 47.5% of women wanted larger breasts than they currently had, 23.2% wanted smaller breasts, and 29.3% were satisfied with their current breast size. There were significant cross-national differences in mean ideal breast size and absolute breast size dissatisfaction, but effect sizes were small (η2 = .02-.03). The results of multilevel modelling showed that greater Neuroticism, lower Conscientiousness, lower Western media exposure, greater local media exposure, lower financial security, and younger age were associated with greater breast size dissatisfaction across nations. In addition, greater absolute breast size dissatisfaction was associated with greater weight and appearance dissatisfaction, poorer breast awareness, and poorer psychological well-being across nations. These results indicate that breast size dissatisfaction is a global public health concern linked to womenâs psychological and physical well-being
The Breast Size Satisfaction Survey (BSSS): Breast size dissatisfaction and its antecedents and outcomes in women from 40 nations
The Breast Size Satisfaction Survey (BSSS) was established to assess women's breast size dissatisfaction and breasted experiences from a cross-national perspective. A total of 18,541 women were recruited from 61 research sites across 40 nations and completed measures of current-ideal breast size discrepancy, as well as measures of theorised antecedents (personality, Western and local media exposure, and proxies of socioeconomic status) and outcomes (weight and appearance dissatisfaction, breast awareness, and psychological well-being). In the total dataset, 47.5 % of women wanted larger breasts than they currently had, 23.2 % wanted smaller breasts, and 29.3 % were satisfied with their current breast size. There were significant cross-national differences in mean ideal breast size and absolute breast size dissatisfaction, but effect sizes were small (?2 = .02â.03). The results of multilevel modelling showed that greater Neuroticism, lower Conscientiousness, lower Western media exposure, greater local media exposure, lower financial security, and younger age were associated with greater breast size dissatisfaction across nations. In addition, greater absolute breast size dissatisfaction was associated with greater weight and appearance dissatisfaction, poorer breast awareness, and poorer psychological well-being across nations. These results indicate that breast size dissatisfaction is a global public health concern linked to women's psychological and physical well-being. © 2020 Elsevier Lt