Issue |
A&A
Volume 515, June 2010
|
|
---|---|---|
Article Number | A93 | |
Number of page(s) | 11 | |
Section | Stellar atmospheres | |
DOI | https://doi.org/10.1051/0004-6361/200913897 | |
Published online | 15 June 2010 |
Behavior of Li abundances in solar-analog stars![[*]](/icons/foot_motif.png)
II. Evidence of the connection with rotation and stellar activity
Y. Takeda1 - S. Honda2 - S. Kawanomoto1 - H. Ando1 - T. Sakurai1
1 - National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
2 - Gunma Astronomical Observatory, 6860-86 Nakayama, Takayama-Mura, Agatsuma-gun, Gunma 377-0702, Japan
Received 18 December 2009 / Accepted 2 February 2010
Abstract
Context. We previously attempted to ascertain why the Li I 6708
line-strengths of Sun-like stars differ so significantly despite the
superficial similarities of stellar parameters. We carried out a
comprehensive analysis of 118 solar analogs and reported that a
close connection exists between the Li abundance (
)
and the line-broadening width (
;
mainly contributed by rotational effect), which led us to conclude that
stellar rotation may be the primary control of the surface
Li content.
Aims. To examine our claim in more detail, we study whether the
degree of stellar activity exhibits a similar correlation with the
Li abundance, which is expected because of the widely believed
close connection between rotation and activity.
Methods. We measured the residual flux at the line center of the strong Ca II 8542 line,
r0(8542), known to be a useful index of stellar
activity, for all sample stars using newly acquired spectra in this
near-IR region. The projected rotational velocity (
)
was estimated by subtracting the macroturbulence contribution from
that we had already established.
Results. A remarkable (positive) correlation was found in the
versus (vs.)
r0(8542) diagram as well as in both the
r0(8542) vs.
and
vs.
diagrams,
as had been expected. With the confirmation of rotation-dependent
stellar activity, this clearly shows that the surface
Li abundances of these solar analogs progressively decrease as the
rotation rate decreases.
Conclusions. Given this observational evidence, we conclude that
the depletion of surface Li in solar-type stars, probably caused
by effective envelope mixing, operates more efficiently as stellar
rotation decelerates. It may be promising to attribute the
low-Li tendency of planet-host G dwarfs to their different
nature in the stellar angular momentum.
Key words: stars: abundances - stars: activity - stars: atmospheres - stars: solar-type - stars: rotation
1 Introduction
Since Li nuclei are burned and destroyed on their arrival at the hot
stellar interior (
K), we can gain valuable
information from the surface Li composition of a star about the past
history and the physical mechanism of stellar envelope mixing.
It has been known, however, that Li abundances (
)
in
Sun-like stars exhibits puzzling behaviors:
- a markedly large diversity (by more than
2 dex) of
is seen despite the similarity of stellar parameters;
- planet-host stars tend to show appreciably lower
than non-planet-host stars (cf. Israelian et al. 2004, 2009).

To elucidate this problem, Takeda et al. (2007,
hereinafter referred to as Paper I) conducted an extensive
high-precision study of stellar parameters as well as of
for 118 solar analogs and found that
values,
exhibiting a large dispersion themselves, are closely correlated
with the line-width, which is characterized by the macroscopic velocity
dispersion (
)
including the rotational as well as the
macroturbulent broadening effect.
We then speculated that
(equatorial rotation velocity)
would be the most important factor affecting
,
since the star-to-star variation in
may be responsible for the spread in
,
any
considerable fluctuation in the macroturbulent velocity
field among similar solar-type stars being difficult to imagine.
The motivation of the present paper, the second in a series,
is to check (or substantiate) the hypothesis that
stellar rotation is the decisive factor
which determines the surface Li content of solar-analogs.
One useful way to accomplish this would be to examine
the stellar activity, which is considered to be of dynamo origin
and thus deeply related to the intrinsic rotational rate. That is,
if we could confirm that
is closely correlated with
the degree of activity, our speculation would be reasonably justified.
As an indicator of stellar activity, we adopt r0(8542) (
), which is the residual
flux (normalized by the continuum) at the line center of
Ca II 8542.09, the strongest line of the near-IR 8498/8542/8662
triplet of mulptiplet 2 for the 2D-2P
transition.
This is known to reflect the chromospheric activity of a star;
i.e., as the activity is enhanced, the core flux increases
because of the greater amount of filled-in emission from the chromosphere
(see, e.g., Linsky et al. 1979). This quantity is known to be well correlated with the more traditional Ca II H+K emission index (
)
and thus serves as a useful tool
for diagnosing the activity level of late-type stars (e.g.,
Foing et al. 1989; Chmielewski 2000; Busà et al. 2007).
In this study we aim to determine r0(8542) (a measure of
stellar activity)
for each of the 118 stars studied in Paper I (a bona-fide sample of
solar analogs), based on our new spectroscopic data obtained at
Okayama Astrophysical Observatory, and examine whether or not
they show any correlation with
,
to test our conclusion in Paper I.
The remainder of this paper is organized as follows.
In Sect. 2, we describe the observational material and the measurement
of r0(8542). Before discussing the results of stellar activity,
the projected rotational velocity (
)
for each star is
derived in Sect. 3 by appropriately subtracting the contribution of
macroturbulence from the macrobroadening parameter (
)
discussed in Paper I. The discussion about the resulting
relationship between r0(8542),
,
and
is presented in Sect. 4, where we show that the arguments
in Paper I have been confirmed, and our conclusions are summarized
in Sect. 5. Two additional appendices are included.
Appendix A describes the results of our reanalysis of stellar
parameters (including Li abundance) for HIP 41484, since another star
(actually HIP 41184) was erroneously observed and analyzed as if it
were HIP 41484 in Paper I. Appendix B is devoted to
discussing the sensitivity difference between two representative
activity indicators, Ca II triplet in near-IR (multiplet 2)
and Ca II H+K lines in violet region (multiplet 1), based on
some test results of non-LTE line profiles simulated with trial models.
2 Residual line-center flux of Ca II 8542
To acquire data for studying stellar activities from Ca II
near-IR triplet, the observations of 118 solar-analog stars (the same sample
as in Paper I) were carried out in five different months (2007 February and
April; 2008 May, August, and December) by using the HIgh-Dispersion Echelle
Spectrograph (HIDES; Izumiura 1999) at the coudé focus of the 188 cm reflector of Okayama Astrophysical Observatory (OAO).
This HIDES, equipped with a 4K 2K CCD detector
at the camera focus, enabled us to obtain an echellogram covering
the wavelength range
of
7600-8800 Å with a resolving power of
(for the normal slit width of 200
m) in the mode of red
cross-disperser. The observational dates for each of
the 118 stars are given in Table 1.
The data reduction (bias subtraction, flat-fielding,
aperture-determination, scattered-light subtraction,
spectrum extraction, wavelength calibration, continuum normalization)
was performed using the ``echelle'' package of IRAF. Several spectral frames taken on a night were coadded to improve the signal-to-noise ratio, values as high as
being finally accomplished in most cases.
![]() |
Figure 1: Example of our HIDES spectrum (for the case of HIP 7918) around the region of Ca II 8498/8542/8662 triplet lines, where spectra of two adjacent orders (66 and 67) are involved. Note that the strongest line (at 8542.09 Å) among the three, whose central depth was used for estimating the stellar activity, is located near to the edge of each spectrum. a) Unnormalized raw spectrum; b) Normalized spectrum with respect to the continuum level. |
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An example spectrum of the Ca II triplet region is shown in
Fig. 1 (for HIP 7918). Unfortunately, the strongest
Ca II line
at 8542. 09 Å, which we use for diagnosing the stellar
activity, is situated close to the edge of the spectral order. Although
this did not cause any essential disadvantage for the present purposes,
we realized that, because of the difficulty in empirically determining
the precise continuum level, a careful readjustment of the continuum
normalization was necessary, which we carried out using Kurucz
et al.'s (1984) solar spectrum atlas as a reference standard. That is, the wing
region (
Å, where
is
the distance from the line center of 8542.09 Å) of each star's
spectrum was adjusted so as to match the corresponding wing of the
reference solar spectrum. This procedure worked satisfactorily well
for all the program stars, as they are analogous to the Sun.
These reduced normalized spectra of the core region are displayed in Fig. 2 for all 118 stars (plus Moon), and the superposition of all the core-region spectra is depicted in Fig. 3. The resulting values of the residual flux at the line center of Ca II 8542,
,
are
summarized in Table 1.
3 Rotational velocity from line width
![]() |
Figure 2: Display of the Ca II 8542 line spectra for all the 118 program stars (along with the Moon/Sun). The wavelength scale of all stellar spectra is adjusted to the laboratory frame by correcting the radial velocity shifts. The HIP numbers are indicated in the figure. |
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![]() |
(1) |
where












![]() |
(2) |
Thus obtained

While any high accuracy (e.g., compared to the case of detailed Fourier
analysis of line profiles) cannot be expected in these
values, given the rough assumptions involved, we consider that they are
surely of the correct order-of-magnitude and practically useful.
Figure 4 shows the comparison of our
results
with the data of Nordström et al. (2004) and Valenti & Fisher (2005), from which we can recognize an almost reasonable consistency, even though some slight systematic trend of deviation is seen.
4 Results and discussion
4.1 Rotation-lithium-activity connection
![]() |
Figure 3:
Overplot of the core-region (within |
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The results of comparisons between
r0(8542),
,
and
are depicted in Figs. 5a, d, and g, respectively.
In Fig. 5a, we can see that
r0(8542) is closely correlated with
(i.e., chromospheric activity is enhanced with increasing rotational velocity), which matches the reasonable belief that
activity is related to rotation-induced stellar dynamo. Figures 5d and g clearly show evidence of the result
we attempt here to prove: the surface Li content (
)
tends
to decline with a decrease in stellar activity (r0)
as well as in rotational rate (
)
. Since the comparatively higher rotator (
km s-1) with rather enhanced activity (
)
have Li abundances close to the solar-system value of
,
from which
progressively decreases with decreasing
as well as
r0(8542), we can confidently state that Li becomes increasingly depleted as the rotation is reduced
in these solar-analog stars.
We should here recall that the rotational velocity
(or angular momentum) is closely related to other parameters,
such as the effective temperature (
)
or the stellar age (age),
because the deceleration of the rotation rate must be more effective
for lower
stars with thicker convection zones,
and older stars should have decelerated more than younger ones.
As implied by Figs. 5b, e, h (
-dependence) and
Figs. 5c,f, and i (age-dependence), such tendencies are
recognized in the sense that rotational velocities tend to be
decelerated more (or alternatively, activities as well as Li abundances
tend to be lower) for older, cooler stars. However, since these trends
are not so tight as those seen in the mutual correlations between
r0(8542),
,
and
(Figs. 5a,
d, and g), we may regard stellar rotation as the most important factor
in controlling the surface Li abundance as well as the
chromospheric activity among the various influential parameters.
4.2 Angular momentum and envelope mixing
![]() |
Figure 4:
Comparison of the
|
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![]() |
Figure 5:
Diagrams showing the correlation between the key physical parameters of
|
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In contrast, Israelian et al. (2009) could not find any
meaningful Li vs. activity correlation or any tendency
toward markedly small
for planet-harboring stars,
while they confirmed the low-Li tendency of planet-host stars
in a more convincing manner.
We note, however, that their discussion is based on
the data of stars with comparatively low-
(
3 km s-1) as well as low-activity
(
which corresponds to
according to Fig. 7)
since their sample of planet-host stars are distributed
across a limited parameter range (cf. their Figs. 2a, b).
It is difficult to discuss any existence of
parameter correlations in this low-rotation/activity region
because of the progressive increase in the relative importance
of errors. The relations that we have found between
,
,
and
(8542)
(being manifest when viewed over a rather wide range of
these parameters; cf. Fig. 5a, d, g) would become appreciably
unclear when we confine ourselves to this restricted region.
Therefore, we can neither exclude nor accept their result
based on their data alone (especially since they used imhomogeneous
literature data of
and
collected
from several references). To settle this issue, far more precise
evaluation of the stellar rotation rate as well as the stellar activity
would be needed (e.g., direct determination of the rotation period
by detecting the modulation of activity indicator based on
long-term observations).
After recognizing that a lithium deficiency is more likely
to take place in slower-rotation stars or planet-host stars,
the next task is to find a reasonable explanation.
Several possibilities for a rotation-mixing connection
have been proposed, such as a turbulent diffusion mixing caused
by magnetic rotational braking and an envelope mixing triggered
by tidal forces from planets (see Gonzalez (2008) or
Israelian et al. (2009) and the quoted references therein).
Based on detailed theoretical simulations, Bouvier (2008) showed
that slow rotators develop a high degree of differential rotation
between the radiative core and the convective envelope,
eventually promoting lithium depletion by enhanced mixing,
while fast rotators experience little similar core-envelope
decoupling. The Li-deficient tendency in planet-host stars may
thus be caused by their slow rotation resulting from a long lasting
star-disk interaction during the pre-main sequence phase.
This line of theoretical approach should be pursued further.
In any case, we should bear in mind that the observed evidence
of
relation does not necessarily
imply a direct physical connection, but may be the result
of a long complex evolution involving different phases (such as
the pre-main sequence).
4.3 Sensitivity of Ca II 8542 as an activity index
We point out problems that remain to be clarified.
We are confident about the global rotation-activity-lithium relation
in the regions of 3 km s
km s-1,
,
and
,
as shown
in Figs. 5a, d, and g. However, little can be said about
the comparatively low-rotation/activity/Li regions of
km s-1,
,
and
,
where
r0(8542) tends to converge for
the value of
0.2, and
as well as
are indefinite because they are close to the detection limit.
This situation is apparent in the histograms of
r0(8542),
,
and
shown in Figs. 6a-c.
How could this large dispersion in
(of more than
1 dex)
be explained at
,
despite
r0(8542)being stabilized at
0.2 (cf. Fig. 2d)?
In our opinion, this implies that the core flux of
Ca II 8542 line is no longer a useful indicator;
i.e., this line is too insensitive to any change in activity
at this low-activity level. We confirmed by means of our
non-LTE line-formation calculation (cf. Appendix B) that
the core-flux of Ca II 8542 is not so sensitive to a mild
chromospheric temperature rise (unless the temperature becomes
sufficiently high to reach a certain threshold level; cf. Fig. B.1c),
which makes itself rather unsuitable to studying the stellar activity
at a lower level. This must be the reason for the convergence
of
r0(8542) at 0.2.
In contrast, our non-LTE calculation suggested that the core
emission of Ca II K line at 3934
is sensitive
to the chromospheric temperature enhancement of any degree (cf. Fig. B.1b),
from which we may conclude that Ca II H+K violet lines are
more useful and practical (than Ca II near-IR triplet lines) at least
for investigating the mild stellar activity of comparatively slow rotators.
We can see from Fig. 7 that, while a reasonable
correlation exists between
r0(8542) and
index
(measure of the core emission strength of Ca II H+K lines),
still exhibits an appreciable dispersion around
-5, whereas
r0(8542) stabilizes at
0.2.
This means that we still may have a chance to study the
rotation-activity-lithium connection of comparatively slow
rotators (
km s-1, where Ca II IR
triplet is no more effective) by studying the Ca II H+K lines.
Additional investigation along these lines would be
worthwhile as we proceed to the next step.
![]() |
Figure 6:
Histograms showing the distributions of a)
r0(8542); b)
|
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![]() |
Figure 7:
Correlation of the
r0(8452) values determined in this study with the
|
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5 Conclusion
In our previous study of Paper I, we carried out a comprehensive spectroscopic analysis of 118 solar analogs to clarify why the strengths of Li I 6708 line in these Sun-like stars are considerably diversified despite that they have stellar parameters quite similar to each other, and interestingly found a close relationship between the Li abundance and its line-width. We then proposed that stellar rotation may be the most important parameter in determining the surface Li content.
In this paper, we have tried to test this hypothesis
by examining whether any correlation exists between
the stellar activity and the Li abundance, as expected
because of the widely believed rotation-activity connection.
As an indicator of stellar activity, we used the residual line-center
flux of the strong Ca II 8542 line (r0), which was measured
from the high-dispersion near-IR spectra obtained with the 188 cm
reflector and the HIDES spectrograph at Okayama Astrophysical Observatory.
The projected rotational velocity (
)
was
reasonably accurately estimated by subtracting the contribution of the
macroturbulence effect from the line-broadening width (
)
as we already established in Paper I.
Clear correlations have been confirmed in the diagrams
vs.
r0(8542),
r0(8542) vs.
,
and
vs.
,
which support the arguments that (1) the stellar activity
surely depends upon the rotational rate,
and that (2) the atmospheric Li abundance of solar-analog stars
declines progressively as the rotational velocity decreases.
We thus concluded that a Li-depletion mechanism in these Sun-like stars, most probably caused by effective envelope mixing, operates more efficiently as the stellar rotation slows down. In this context, it may be interesting/enlightening to interpret the observational finding of a low-Li tendency of planet-host G dwarfs within the framework of the rotational properties (i.e., difference in the angular momentum), as stated in the theoretical prediction by Bouvier (2008). Additional detailed investigations along those lines would be worthwhile.
However, the cause of this interconnection, which is found
for comparatively high-rotation/activity/Li stars, remains unclear
for the group of stars with low-rotation/activity/Li, where
r0(8542)
tends to converge and stabilize at 0.2 and can no longer be
a useful activity indicator. Since we found from our non-LTE calculation
that Ca II H+K violet lines at 3968/3934
are more sensitive
and useful (than Ca II IR triplet lines) for investigating the
mild stellar activity of comparatively slow rotators, it would be
beneficial to revisit this problem by studying these Ca II H+K lines
in greater detail.
We thank the staff of the Okayama Astrophysical Observatory for their kind and elaborate support in the observations.Constructive comments from an anonymous referee concerning the interpretation of low-Li tendency in planet-host stars are also acknowledged.
Appendix A: Reanalysis of HIP 41484
![]() |
Figure A.1:
Spectrum fitting analysis applied to selected wavelength regions of
HIP 41484. The observed and theoretical spectra are shown by open
(line-connected) circles and solid lines, respectively. a) 6591-6599 |
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In the course of this study, we noticed that the near-IR spectrum
of HIP 41484 obtained for this study and the red-region
spectrum used in Paper I were apparently inconsistent with each other.
After careful inspection of the observational information
(e.g., telescope pointing ), we then realized that the red spectrum
obtained for this star in 2005 November 26 was not that
of HIP 41484 but that of HIP 41184
(which was also one of our solar-analog targets); i.e.,
we had mistakenly observed the incorrect star because of the similarity
in their HIP number
.
Since an erroneous spectrum was eventually used in Paper I, all the
spectrum-related quantities derived therein were also wrong. We thus
carried out an entire reanalysis of HIP 41484 based on the new spectrum
used for this study, where a long wavelength range of 6300-10 000 was fortunately available (thanks to the 3 mosaicked CCDs; cf. footnote 2)
in addition to the main region of 7600-8800
including the Ca II triplet. The atmospheric parameters (
,
,
,
and [Fe/H]) were derived from the Fe I and Fe II lines
6300-7600
region. Since the 6080-6089
region
used in Paper I to evaluate the line-broadening width by the
spectrum-fitting method was not available in the present case,
we instead used the 6591-6599
region for this purpose (Fig. A.1a). The Li abundance was determined from the Li I doublet at 6708
(Fig. A.1b).
Otherwise, all the relevant stellar parameters were established in the
same way as in Paper I. The results of this reanalysis are
summarized in Table A.1.
Table A.1: Redetermined stellar parameters and physical quantities of HIP 41484.
Appendix B: Ca II H+K doublet and near-IR triplet as stellar-activity indicators
It is well known that the cores of strong Ca II lines,
such as the resonance H+K doublet lines (at 3968 and 3934 )
or the near-IR triplet lines (at 8498/8542/8662
),
reflect the temperature structure of the upper atmosphere
and may be used as useful indicators of chromospheric activity.
However, does any difference exist between these two activity indicators
in their practical applications; do they have any specific strong or
weak points depending on situations?
To answer this, we tried to compute the profiles of
Ca II 3934 and Ca II 8542 lines for several test model
atmospheres with different chromospheric effects,
and examine how the core fluxes of these two lines respond to
the temperature profile of upper atmospheres.
We must take into account non-LTE effects, because
the dilution of the line source function in the upper optically-thin
layer determines the intensity/flux level at the core.
Non-LTE statistical-equilibrium calculations directed specifically
toward studying the formation of these strong Ca II lines
in the chromosphere have been few in number.
Except for the pioneering work on a simple 3-level Ca II model
ion (e.g., Linsky & Avrett 1970 for the H+K lines; Linsky et al. 1979
for the 8542 line), the only relevant non-LTE study quotable here
may be, to our knowledge, that of Andretta et al. (2005),
who computed (based on a model atom comprising 18 Ca I and
5 Ca II levels) the 8498/8542/8662 line profiles for various
solar models including a semi-empirical one with the chromosphere.
We dealt with this problem here using a more detailed atomic
model of calcium (111/50 terms and 2376/313 radiative transitions
for Ca I/Ca II), comprising up to
Ca I 4 16
3D (48830 cm-1 from the ground level) and Ca II 3p6 16d 2D (93895 cm-1 from the ground level), which was constructed from the atomic-line database compiled by Kurucz & Bell (1995). The electron collision cross-sections relevant to the lowest 7 terms of Ca II were taken from Burgess et al. (1995). The data from TOPbase (Cunto & Mendoza 1992) were adopted for the photoionization cross-sections for the lowest 7 and 10 terms of Ca I and Ca II, respectively. As for other computational details (e.g., electron-collision rates as well as
photoionization rates for the remaining terms not mentioned above,
collisional ionization rates, treatment of collisions
with neutral-hydrogen atoms), we followed the recipe
described in Sect. 3.1.3 of Takeda (1991).
![]() |
Figure B.1: Test simulations for the core profiles of Ca II 3934 (K) line and Ca II 8542 line, based on the non-LTE calculations carried out on three model atmospheres (Models C, M, and E) with different temperature structures at the upper atmosphere. a) Temperature profiles of Models C, M, and E. b) Simulated (flux) profiles of the Ca II 3934 line; c) simulated (flux) profiles of the Ca II 8542 line. In panels b) and c), Kurucz et al.'s (1984) solar flux spectra are also indicated by open circles. |
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We tested three solar atmospheric models (
K,
,
[Fe/H] = 0.0) that have different temperature profiles
only at the upper layer of
.
Model C has
a chromospheric temperature structure similar to that of the semi-empirical
solar model of Maltby et al. (1986). Model E is equivalent to
Kurucz's (1979) ATLAS6 solar model (without any temperature rise), and Model M corresponds to the mean of these two (cf. Fig. B.1a). The pressure/density structures of these models were obtained by integrating the equation of hydrostatic equilibrium.
We refer to Sect. 2.1 of Takeda (1995b)
for more details about how Models C and E were constructed.
We applied a depth-dependent microturbulence by adopting the turbulent
velocity fields given in Table 11 of Maltby et al. (1986).
The resulting profiles of Ca II 3934 and 8542 lines are
depicted in Figs. B.1b, c, respectively, where the corresponding
solar flux spectra of Kurucz et al. (1984)
are also shown for comparison. It can be seen that the computed
profiles for Model C, which is likely to be the most realistic
among the three, do not reproduce the true solar spectra well (i.e.,
the core flux level is too high), indicating that our modeling is still
imperfect. However, our intention here is not to accomplish excellent
fitting between theory and observation, but to ascertain/determine
whether and how the sensitivity to the upper temperature differs
between these two lines. From this standpoint, we can recognize an
important result in these figures: The strength of the core emission in
the
Ca II 3934 line progressively increases in accordance with
the temperature rise in the upper layer as
Model E
Model M
Model C (Fig. B.1b).
In contrast, the residual core flux of Ca I 8542 line barely
differs for Models E and M, while that for Model C is
appreciably higher (Fig. B.1c), which means that this indicator
is not very useful for studying the moderate temperature enhancement
(mild chromospheric activity) because of its rather inefficient
response until the temperature rise goes over a certain threshold level.
Consequently, we may conclude that those who intend to study the
nature of comparatively mild stellar activity in slower rotators
should use the Ca II H+K lines at 3934/3968
,
rather than the Ca II triplet lines at 8498/8542/8662
.
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Table 1: Activity index, rotation, Li abundance, age, and the atmospheric parameters.
Footnotes
- ... stars
- Based on observations carried out at Okayama Astrophysical Observatory (Okayama, Japan).
- ... activity
- Of course, this
r0(8542) index depends not only on the chromospheric activity but also
on atmospheric parameters such as
(effective temperature),
(surface gravity), and [Fe/H] (metallicity) (e.g., Mallik 1997; Chmielewski 2000). However, in the present sample of solar analogs similar to each other, the mutual differences of these stellar parameters are of secondary importance and can be neglected to a first approximation.
- ... range
- Since the beginning of 2008, three mosaicked
CCD chips had become newly available in HIDES, resulting in a three-times
wider wavelength coverage than before. Accordingly, for the data of
2008 May, August, and December, spectra in two adjacent wavelength ranges
(6300-7600 Åand 8800-10 000 Å) were also recorded in
addition to the target region of 7600-8800
.
- ... IRAF
- IRAF is distributed by the National Optical Astronomy Observatories, which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.
- ...
)
- We should remark that the residual intensity at the core gets more or less
raised as
becomes higher due to the blurring effect (caused by correspondingly wider rotational broadening function being convolved). However, we can see from Fig. 5a (see the dotted line therein) that this effect is quantitatively insignificant compared to the main trend (symbols) which must thus be real.
- ... number
- As a result, HIP 41184 was unintentionally observed twice. In Figs. 6 and 8 in Paper I, the two spectra labeled as ``41184'' and ``41484'' actually correspond to the same star (HIP 41184).
- ... number
- More precisely, several other non-LTE studies of calcium lines in late-type stars (e.g., Watanabe & Steenbock 1985; Drake 1991; Jørgensen et al. 1992; Mashonkina et al. 2007), focusing mainly on non-LTE abundance corrections, do not explicitly address the chromospheric effect (core emission) on the formation of these activity-sensitive Ca II lines under question.
All Tables
Table A.1: Redetermined stellar parameters and physical quantities of HIP 41484.
Table 1: Activity index, rotation, Li abundance, age, and the atmospheric parameters.
All Figures
![]() |
Figure 1: Example of our HIDES spectrum (for the case of HIP 7918) around the region of Ca II 8498/8542/8662 triplet lines, where spectra of two adjacent orders (66 and 67) are involved. Note that the strongest line (at 8542.09 Å) among the three, whose central depth was used for estimating the stellar activity, is located near to the edge of each spectrum. a) Unnormalized raw spectrum; b) Normalized spectrum with respect to the continuum level. |
Open with DEXTER | |
In the text |
![]() |
Figure 2: Display of the Ca II 8542 line spectra for all the 118 program stars (along with the Moon/Sun). The wavelength scale of all stellar spectra is adjusted to the laboratory frame by correcting the radial velocity shifts. The HIP numbers are indicated in the figure. |
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Overplot of the core-region (within |
Open with DEXTER | |
In the text |
![]() |
Figure 4:
Comparison of the
|
Open with DEXTER | |
In the text |
![]() |
Figure 5:
Diagrams showing the correlation between the key physical parameters of
|
Open with DEXTER | |
In the text |
![]() |
Figure 6:
Histograms showing the distributions of a)
r0(8542); b)
|
Open with DEXTER | |
In the text |
![]() |
Figure 7:
Correlation of the
r0(8452) values determined in this study with the
|
Open with DEXTER | |
In the text |
![]() |
Figure A.1:
Spectrum fitting analysis applied to selected wavelength regions of
HIP 41484. The observed and theoretical spectra are shown by open
(line-connected) circles and solid lines, respectively. a) 6591-6599 |
Open with DEXTER | |
In the text |
![]() |
Figure B.1: Test simulations for the core profiles of Ca II 3934 (K) line and Ca II 8542 line, based on the non-LTE calculations carried out on three model atmospheres (Models C, M, and E) with different temperature structures at the upper atmosphere. a) Temperature profiles of Models C, M, and E. b) Simulated (flux) profiles of the Ca II 3934 line; c) simulated (flux) profiles of the Ca II 8542 line. In panels b) and c), Kurucz et al.'s (1984) solar flux spectra are also indicated by open circles. |
Open with DEXTER | |
In the text |
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