J/A+A/682/A136 Activity indexes analysis (Claudi+, 2024)
The GAPS Programme at TNG. LI. Investigating the correlations between transiting
system parameters and host chromospheric activity.
Claudi R., Bruno G., Fossati L., Lanza A.F., Maggio A., Micela G.,
Maldonado J., Benatti S., Biazzo K., Bignamini A., Cabona L., Carleo I.,
Danielski C., Desidera S., Malavolta L., Mancini L., Montalto M.,
Nardiello D., Rainer M., Scandariato G., Sozzetti A., Cosentino R.,
Covino E., Di Fabrizio L., Ghedina A., Lorenzi V., Molinari E.,
Molinaro M., Pagano I., Piotto G., Poretti E.
<Astron. Astrophys., 682, A136 (2024)>
=2024A&A...682A.136C 2024A&A...682A.136C (SIMBAD/NED BibCode)
ADC_Keywords: Stars, activity ; Stars, double and multiple ; Exoplanets ;
Optical ; Effective temperatures
Keywords: planets and satellites: fundamental parameters -
planet-star interactions - stars: activity - planetary systems
Abstract:
Stellar activity is the most relevant types of astrophysical noise
that affect the discovery and characterization of extrasolar planets.
On the other hand, the amplitude of stellar activity could hint at an
interaction between the star and a close-in giant planet. Progress has
been made in recent years in understanding how to deal with stellar
activity and search for observational evidence of star-planet
interactions.
The aim of this work is to characterize the chromospheric activity of
stars hosting short-period exoplanets by studying the correlations
between the chromospheric emission (CE) in the CaII H&K and the
planetary parameters.
We measured CE in the CaII H&K lines using more than 1900
high-resolution spectra of a sample composed of 76 targets, observed
with the HARPS-N spectrograph between 2012 and 2020. We transformed
the fluxes into bolometric- and photospheric-corrected chromospheric
emission ratios, R'HK. Furthermore, we completed the sample of hosts
digging for data in previous works. Stellar parameters Teff, B-V,
and V were retrieved homogeneously from the Gaia DR3. Then, M*, R*,
and ages were determined from isochrone fitting. We retrieved
planetary data from the literature and catalogs. The search for
correlations between the log(R'HK) and planetary parameters have
been performed through both Spearman's rank and its statistics as well
as the more sophisticated Gaussian mixture model method.
We found that the distribution of log(R'HK) for the transiting
planet hosts is different from the distribution of field main-sequence
and sub-giant stars. The log(R'HK) of planetary hosts is correlated
with planetary parameters proportional to the planetary radius to the
power of n (RPn, indicating a common origin for the correlations.
The statistical analysis has also highlighted four clusters of host
stars with different behavior in terms of their stellar activity with
respect to the planetary surface gravity. Some of the host stars have
a value of log(R'HK) that is lower than the basal level of activity
for main sequence stars. The planets of these systems are very close
to filling their Roche lobe, suggesting that they evaporate through
hydrodynamic escape under the strong irradiation of the host star,
creating shrouds that absorb the core of the chromospheric resonance
lines.
Description:
For each of the 131 stars in the sample, we obtained the stellar
parameters (Teff, B-V, V in a homogeneous way, exploiting the Gaia DR3
data release, 2022, Cat. I/355). The S-index and the corresponding
log(R'HK)N median values are reported for each object of the GAPS
sample in Table 2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 113 131 For all systems, the table lists Gaia DR3 id.,
and (B-V), and Teff obtained by Gaia
Collaboration (2018A&A...616A...1G 2018A&A...616A...1G)
as explained in the text
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
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1- 9 A9 --- System System name
11- 13 A3 --- n_System [abcd, ] Note on System (1)
16- 34 I19 --- GaiaDR3 Gaia DR3 identification number
36- 40 F5.3 mag B-V B-V oolour index
42- 46 F5.3 mag e_B-V ? B-V oolour index error
49- 52 I4 K Teff Effective temperature
54- 56 I3 K e_Teff Effective temperature error
58- 59 I2 --- r_Teff ? Effective temperature reference (3)
62- 66 F5.3 --- SMWO SMWO activity index
68- 72 F5.3 --- e_SMWO ? SMWO activity index error
74- 75 I2 --- r_SMWO ? SMWO activity index reference (3)
78- 84 F7.4 --- log(R'HK)N log(R'HK) activity index obtained with
Noyes et al. (1984ApJ...279..763N 1984ApJ...279..763N)
procedure (2)
86- 91 F6.4 --- e_log(R'HK)N ? log(R'HK) activity index obtained with
Noyes et al. (1984ApJ...279..763N 1984ApJ...279..763N)
procedure error
94-100 F7.4 --- log(R'HK)M log(R'HK) activity index obtained with
Mittag et al. (2013A&A...549A.117M 2013A&A...549A.117M)
procedure (2)
102-107 F6.4 --- e_log(R'HK)M ? log(R'HK) activity index obtained with
Mittag et al. (2013A&A...549A.117M 2013A&A...549A.117M)
procedure error
109-113 F5.3 10+5 rms ?=- rms of the several measured time series
(R'HKx105rms)
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Note (1): Notes as follows:
a = The R-indices obtained with the relation of Mittag et al.
(2013A&A...549A.117M 2013A&A...549A.117M) are derived in the color range of 0.44<B-V<1.6.
Nevertheless, we give values for all the objects in our samples, and
values for spectral types out of this color range should be taken with
a pinch of salt.
b = Also known as HD147506
c = Also known as WASP-40
d = Also known as HAT-P-10
Note (2): The CaII H&K line strength is listed for both the original GAPS sample
and the sample obtained by literature. We report the classical value
(Noyes et al., 1984ApJ...279..763N 1984ApJ...279..763N) of the activity as obtained in this
work or in the literature in log(R'HK)N column while in the the values
corrected with the Mittag et al. (2013A&A...549A.117M 2013A&A...549A.117M) procedure as described
in Sect. 4.2 are reported in log(R'HK)M column.
Note (3): References as follows:
1 = Wright et al. (2004AJ....128.1273W 2004AJ....128.1273W)
2 = Knutson et al. (2010ApJ...720.1569K 2010ApJ...720.1569K)
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5 = Beky et al. ( 2011ApJ...734..109B 2011ApJ...734..109B, Cat. J/ApJ/734/109)
6 = Buchhave et al. (2011ApJ...733..116B 2011ApJ...733..116B, Cat. J/ApJ/733/116)
7 = Hartman et al. (2011ApJ...742...59H 2011ApJ...742...59H, Cat. J/ApJ/742/59)
8 = Bakos et al. (2012AJ....144...19B 2012AJ....144...19B, Cat. J/AJ/144/19)
9 = Sato et al. (2012PASJ...64...97S 2012PASJ...64...97S)
10 = Hartman et al. (2012AJ....144..139H 2012AJ....144..139H, Cat. J/AJ/144/139)
11 = Hartman et al. (2014AJ....147..128H 2014AJ....147..128H, Cat. J/AJ/147/128)
12 = Howard et al. (2011ApJ...730...10H 2011ApJ...730...10H)
13 = Dumusque et al. (2014ApJ...789..154D 2014ApJ...789..154D, Cat. J/ApJ/789/154)
14 = Winn et al. (2011ApJ...741L...1W 2011ApJ...741L...1W)
15 = Bonomo et al. (2012A&A...538A..96B 2012A&A...538A..96B)
16 = Malavolta et al. (2017AJ....153..224M 2017AJ....153..224M)
17 = Gautier et al. (2012ApJ...749...15G 2012ApJ...749...15G, Cat. J/ApJ/749/15)
18 = Borucki et al. (2012ApJ...745..120B 2012ApJ...745..120B)
19 = Marcy et al. (2014ApJS..210...20M 2014ApJS..210...20M, Cat. J/ApJS/210/20)
20 = Borucki et al. (2013Sci...340..587B 2013Sci...340..587B)
21 = Gilliland et al. (2013ApJ...766...40G 2013ApJ...766...40G)
22 = Pepe et al. (2013Natur.503..377P 2013Natur.503..377P)
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24 = Albrecht et al. (2012ApJ...744..189A 2012ApJ...744..189A)
25 = Brown et al. (2012MNRAS.423.1503B 2012MNRAS.423.1503B, Cat. J/MNRAS/423/1503)
26 = Anderson et al. (2011A&A...534A..16A 2011A&A...534A..16A, Cat. J/A+A/534/A16)
27 = Triaud et al. (2011A&A...531A..24T 2011A&A...531A..24T, Cat. J/A+A/531/A24)
28 = Maxted et al. (2011PASP..123..547M 2011PASP..123..547M)
29 = Lendl et al. (2012A&A...544A..72L 2012A&A...544A..72L, Cat. J/A+A/544/A72)
30 = Hebrard et al. (2013A&A...549A.134H 2013A&A...549A.134H, Cat. J/A+A/549/A134)
31 = Anderson et al. (cw2014MNRAS.445.1114A, Cat. J/MNRAS/445/1114)
32 = Staab et al. (2017MNRAS.466..738S 2017MNRAS.466..738S)
33 = Lendl et al. (2014A&A...568A..81L 2014A&A...568A..81L, Cat. J/A+A/568/A81)
34 = Tsantaki et al. (2014A&A...570A..80T 2014A&A...570A..80T)
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History:
From electronic version of the journal
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(End) Patricia Vannier [CDS] 24-Apr-2024