J/A+A/694/A325 Environmental effects on nearby debris discs (Heras+, 2025)
Environmental effects on nearby debris discs.
Heras A.M., Eiroa C., del Burgo C., Marshall J.P., Montesinos B.
<Astron. Astrophys. 694, A325 (2025)>
=2025A&A...694A.325H 2025A&A...694A.325H (SIMBAD/NED BibCode)
ADC_Keywords: Stars, nearby ; Stars, ages ; Photometry, infrared ;
Space velocities
Keywords: circumstellar matter - stars: kinematics and dynamics - ISM: general -
infrared: planetary systems - infrared: stars
Abstract:
We aim to investigate the influence of the interstellar medium (ISM)
on debris discs using a statistical approach. We probe the effect of
the ISM on debris disc occurrence rates and on the morphologies of the
discs.
We used the results of the Herschel Space Observatory DUNES and DEBRIS
surveys of 295 nearby FGK dwarf stars imaged at 100um and 160um.
Most of the 48 debris discs in this sample have small optical depths,
making them more likely to be affected by the interstellar medium
(ISM) compared to optically thick discs. Since the stars of our sample
are located within the Local Interstellar Cloud (LIC), we can infer
that their debris discs encounter similar conditions. This allows us
to use the stellar space velocity, in particular the U component, as a
single indicator of the forces that can act on the debris disc dust
grains when they interact with the ISM. Because older stars show a
larger dispersion of space velocity values, we have investigated the
impact of the debris disc ages on our results.
The observed debris disc occurrence rates show a dependence on the
stellar space velocities as expected under the hypothesis that stars
with larger space velocities have a higher probability of losing their
circumstellar dust. The percentage of sources with debris discs in our
sample reaches a maximum of ~=25% for stars with low values of the
space velocity component |Urel|, relative to the Local ISM, and
decreases monotonically for larger |Urel| values down to the 10%
level. A decrease of the average disc fractional luminosity as a
function of |Urel| is also observed. These dependencies do not
disappear after accounting for the reported higher dispersion of U
values with age. In extended discs, the impact of the ISM could also
explain the trends observed for the debris disc's projected
ellipticities, position angles, and radii with the stellar space
velocities. The fractional luminosities of the debris discs appear to
be correlated with their position angles, suggesting that the effect
of the ISM on the dust content could depend on the disc orientation.
Although these indications may not be fully conclusive on their own,
they collectively reinforce the hypothesis that the ISM influences the
occurrence rates and morphologies of debris discs, thereby motivating
additional research on the impact of the environment.
Description:
The list of stars used in this study was compiled using the results of
the DUNES and DEBRIS surveys proposed as OTKP (Open Time Key
Programmes) to the Herschel Space Observatory, which obtained images
at 100um and 160um of nearby stars, complemented in some cases with
observations at 70um (Matthews et al. 2010A&A...518L.135M 2010A&A...518L.135M; Eiroa et
al., 2013A&A...555A..11E 2013A&A...555A..11E, Cat. J/A+A/555/A11; Montesinos et al.,
2016A&A...593A..51M 2016A&A...593A..51M, Cat. J/A+A/593/A51; Sibthorpe et al.
2018MNRAS.475.3046S 2018MNRAS.475.3046S; Marshall et al. 2021MNRAS.501.6168M 2021MNRAS.501.6168M). The DUNES
sample is sensitivity- and background-limited, and contains FGK
solar-like stars located at d~=20pc. The Sibthorpe et al.
(2018MNRAS.475.3046S 2018MNRAS.475.3046S) sample is volume-limited and consists of FGK
solar-like stars. We have excluded the six cold discs identified in
the DUNES sample by Eiroa et al. (2011A&A...536L...4E 2011A&A...536L...4E), Marshall et
al. (2013A&A...557A..58M 2013A&A...557A..58M) and Krivov et al. (2013ApJ...772...32K 2013ApJ...772...32K). The
maximum distance of the combined samples is 25pc.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 73 295 Full sample
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See also:
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Name Hipparcos (HIP) catalogue number or GJ name
14- 22 E9.3 --- Ldust/L* ? Fractional dust luminosity
24 A1 --- Planets [y] Detected planets (1)
26- 31 F6.2 Gyr Age ? Stellar age
33- 37 F5.2 Gyr b_Age ? Stellar age 16% posterior CDF value
39- 44 F6.2 Gyr B_Age ? Stellar age 84% posterior CDF value
46- 52 F7.2 km/s Uvel Space Velocity component U in Galactic
coordinate system
54- 60 F7.2 km/s Vvel Space Velocity component V in Galactic
coordinate system
62- 67 F6.2 km/s Wvel Space Velocity component W in Galactic
coordinate system
69- 73 A5 --- Ref References (2)
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Note (1): "y" indicates that at least an exoplanet has been detected
Note (2): References are as follows:
For Ldust/L*:
1 = Eiroa et al., 2013A&A...555A..11E 2013A&A...555A..11E, Cat. J/A+A/555/A11
2 = Montesinos et al., 2016A&A...593A..51M 2016A&A...593A..51M, Cat. J/A+A/593/A51
3 = Sibthorpe et al., 2018MNRAS.475.3046S 2018MNRAS.475.3046S
For Space Velocities:
4 = Derived from Gaia Collaboration et al., 2021A&A...649A...1G 2021A&A...649A...1G
5 = Casagrande et al., 2011A&A...530A.138C 2011A&A...530A.138C, Cat. J/A+A/530/A138
6 = Bobylev et al., 2006ARep...50..733B 2006ARep...50..733B, Cat. J/AZh/83/821
7 = Gliese & Jahreiss, 1991, Cat. V/70
For Ages:
8 = Stanford-Moore et al., 2020ApJ...898...27S 2020ApJ...898...27S, Cat. J/ApJ/898/27
9 = Montesinos et al., 2016A&A...593A..51M 2016A&A...593A..51M, Cat. J/A+A/593/A51
For planets: exoplanet.eu
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Acknowledgements:
Ana Heras, ana.heras(at)esa.int
(End) Patricia Vannier [CDS] 15-Jan-2025