A&A 409, 263-274 (2003)
DOI: 10.1051/0004-6361:20030978
P. Gondoin
European Space Agency, ESTEC - Postbus 299, 2200 AG Noordwijk, The Netherlands
Received 13 December 2002 / Accepted 19 June 2003
Abstract
HD 223460 (HR 9024), a chromospherically active late-type giant with
a high X-ray luminosity, was observed by the XMM-Newton space
observatory. Series of lines of highly ionized Fe and several Lyman
lines of hydrogen-like ions and triplet lines of helium-like ions are
visible in the reflection grating spectra, most notably from O and
Ne. Analysis results suggest a scenario where the corona of HD 223460
is dominated by large magnetic structures similar in size to
interconnecting loops between solar active regions but significantly
hotter. The surface area coverage of these active regions may approach
up to 30%. A hypothesis is that the interaction of these
structures themselves induces a flaring activity on a small scale not
visible in the EPIC light curves that is responsible for heating HD 223460 plasma to coronal temperatures of
K. The intense
X-ray activity of HD 223460 is related to its evolutionary position at
the bottom of the red giant branch. It is anticipated that its
rotation will spin down in the future with the effect of decreasing
its helicity-related, dynamo-driven activity and suppressing large-scale magnetic structures in its corona.
Key words: stars: individual: HD 223460 - stars: activity - stars: coronae - stars: evolution - stars: late-type - X-rays: stars
HD 223460 (HR 9024) is a chromospherically active late-type
giant. Cowley & Bidelman (1979) indicate that the Ca II emission in
this star is moderately strong while Bopp (1984) notes that the H and K emission fluxes are quite high, comparable to what is observed in FK
Comae. Feldman (1982) detected HD 223460 as a radio source and
initially suggested that HD 223460, which apparently exhibits no
detectable velocity variation, is an FK Comae type star. Cowley &
Bidelman (1979) classified HD 223460 as a G1 III star but its B - V color is too large for the assigned MK type which suggests unusual
reddening for the distance (Ayres et al. 1998). HD 223460 shows some
Li I absorption (De Medeiros & Lebre 1992), a sign of evolutionary
youth and lack of deep mixing (Wallerstein et al. 1994) consistent
with its spectral type and luminosity class which indicate that the
star recently became a giant. Its rotation velocity (
km s-1; Fekel et al. 1986) is low for an FK Comae type star and
Bopp (1984) suggested that the star could be seen pole-on. This
moderate
of
km s-1 confirmed by Medeiros
& Lebre (1992) is comparable with the photometric rotation period of
23 days measured by Strassmeier & Hall (1988) for a normal
10
giant. Another characteristic of HD 223460 includes an
X-ray luminosity (Singh et al. 1996; Hünsch et al. 1998)
exceptionally high for a red giant, similar to that of an FK comae
type star (Gondoin 1999). I report on analysis results of X-ray
spectra of HD 223460 registered during two observations performed in
July 2000 and in January 2001 by the XMM-Newton
observatory. The observations were conducted with the aim to improve
our understanding of the magnetic activity on HD 223460 by
investigating the origin of its high X-ray luminosity and the
structure of its X-ray corona.
This paper is organized as follows. Section 2 provides the stellar parameters of HD 223460 and compares the evolution status of this star with those of nearby single field giants in light of Hipparcos parallaxes (ESA 1997). Section 3 describes the X-ray observations of HD 223460 and the data reduction procedures. Section 4 then presents the integrated flux measurements and their temporal behavior during the observations. Section 5 describes the spectral analysis of the datasets obtained with the European Photon Imaging Camera (EPIC) and the Reflection Grating Spectrometer (RGS) on board XMM-Newton. Finally, a physical interpretation of the analysis results is proposed in Sect. 6. In this last section, the structure of HD 223460 corona and its possible evolution is discussed within the frame of stellar activity evolution across the Hertzsprung gap.
A differential UBV photometry study performed by Strassmeier & Hall (1988) indicates a V magnitude amplitude variation of 0.065 on HD 223460 presumably due to spot activities in the photosphere of the star. Since reliable measurements of the minimum V magnitude were not found, an upper estimate of the maximum luminosity of HD 223460 was obtained by subtracting the above V amplitude variation from the V Johnson magnitude specified in the Hipparcos catalogue. The visual extinction of the star was calculated by applying Chen et al. (1998) model with the upper distance limit derived from the Hipparcos catalogue. The visual extinction is smaller than the magnitude variation due to rotational modulation by photospheric spots. The absolute magnitude was calculated from the V magnitude, visual extinction and Hipparcos parallax (see Table 1). The stellar luminosity was then derived using the bolometric correction vs. effective temperature data of Flower (1996).
Figure 1 shows the position of HD 223460 in the H-R diagram compared with evolutionary tracks inferred from grids of stellar models with a near solar metallicity (Z=0.02) provided by Schaller et al. (1992). The models use opacities provided by Rogers & Iglesias (1991) and Kurucz (1991) and their convection parameters (i.e. mixing length ratio and overshooting parameter) have been calibrated using the red giant branch (RGB) of a wide range of clusters. The mass of HD 223460 was estimated to 2.8-3.1
from its position with respect to the theoretical evolutionary tracks. The star most likely originates from an early B type, single star as it evolves in the giant domain. Li abundance measurements (Wallerstein et al. 1994) support this scenario where the star has recently become a giant and is crossing the Hertzsprung gap prior the lithium depletion by convective dilution. At a later evolutionary stage when the star ascends the red giant branch, the inward expansion of its convective envelope would be expected to transport Li from the surface to the interior thus reducing its surface abundance.
The radius of HD 223460 was calculated from its luminosity and
effective temperature. The photometric period (P = 23 days;
Strassmeier & Hall 1988) and the radius of the star were then used to
estimate its equatorial velocity (see Table 1). Comparison with the
projected rotational velocity (
km s-1;
de Medeiros & Lebre 1992) derived spectroscopically indicates a large
inclination angle (
)
of the star's polar axis onto the
line of sight. This effect contributes to explain the large rotational
velocity of HD 223460 that is consistent with the hypothesis that the
star is a normal G giant that has evolved from a single B type
progenitor.
Table 1: Top: V magnitude, parallax and absolute magnitude of HD 223460. Middle: spectral type, color indices and effective temperature. Bottom: estimated stellar parameters of HD 223460.
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Figure 1:
H-R diagram of single giants (Gondoin 1999) compared with
evolutionary tracks (Schaller et al. 1992). The dot-dashed
lines from bottom to top describe the evolutionary
tracks of 1 ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Table 2: HD 223460 observation log during XMM-Newton revolutions 107 and 200.
HD 223460 was observed twice by the XMM-Newton space observatory (Jansen et al. 2001), in revolutions 107 on 9 July 2000, and 200 on 10 January 2001 (see Table 2). The satellite observatory uses three grazing incidence telescopes which provide an effective area higher than 4000 cm2 at 2 keV and 1600 cm2 at 8 keV (Gondoin et al. 2000). Three CCD EPIC cameras (Strüder et al. 2001; Turner et al. 2001) at the prime focus of the telescopes provide imaging in a 30 arcmin field of view and broadband spectroscopy with a resolving power of between 10 and 60 in the energy band 0.3 to 10 keV. Two identical RGS reflection grating spectrometers behind two of the three X-ray telescopes allow higher resolution (
to 500) measurements in the soft X-ray range (6 to 38 Å or 0.3 to 2.1 keV) with a maximum effective area of about 140 cm2 at 15 Å (den Herder et al. 2001).
HD 223460 observations were conducted with the EPIC cameras operating in full frame mode (Ehle et al. 2001). RGS spectra were recorded simultaneously. "Thick'' aluminium filters were used in front of the EPIC MOS cameras and "Medium'' thickness aluminium filters were used in front of EPIC p-n cameras to reject visible light. Processing of the raw event dataset was performed using the
"emchain'', "epchain'' and "rgsproc'' pipeline tasks of the XMM-Newton Science Analysis System (SAS version 5.3.0). HD 223460 spectra were built from photons detected within windows of about 60
diameter around the target boresight in the EPIC cameras. The background was estimated on the same CCD chips as the source, within windows of similar sizes which were offset from the source position in an empty field region. The Pulse-Invariant (PI) spectra were rebinned such that each resulting MOS channel had at least 20 counts per bin and each p-n channel had at least 40 counts per bin.
minimization was used for spectral fitting. All fits were performed using the XSPEC package (Arnaud & Dorman 2001). The EPIC and RGS response matrices were generated by the SAS task "rmfgen'' and "rgsrmfgen'' respectively. EPIC p-n, MOS 1 and MOS 2 spectra were fitted together in the 0.3 to 9 keV energy range in revolution 107 and in the 0.3 to 6.5 keV energy range in revolution 200. The upper cut-off of the spectral band was imposed by the decreasing count rate at high energies. The RGS spectra were analysed separately due to their higher spectral resolution in the 0.3-2.1 keV energy range.
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Figure 2: Light curves of HD 223460 during revolutions 107 (left) and 200 (right) obtained with the EPIC p-n camera. In each graph, the upper curve is the count rate within the 0.3 to 2 keV band and the lower curve is the count rate within the 2 to 10 keV band. The events are binned in 300 s time intervals and the background contribution has been subtracted. |
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Figure 2 shows the light curves of HD 223460 obtained during revolution 107 and 200 with the p-n camera after subtraction of background
events. In the 0.3-2 keV energy band, the count rate is about 15%
higher in revolution 107 with an average count rate of
s-1 compared with a count rate of
s-1 in
revolution 200. In the 2-10 keV energy band, the count rate is about 50% higher in revolution 107 with an average count rate of
s-1 compared with a count rate of
s-1 in revolution 200. The 0.3-2 keV over 2-10 keV count rate
ratios are
and
during revolutions 107 and 200
respectively, indicating that the spectrum of HD 223460 was soft
during both observations. The count rate in the low energy band
decreased steadily by
2.3% over 6.7 ksec in revolution 107. It increased steadily by about 5.6% over 1 hour in revolution 200.
Table 3:
X-ray luminosities (corrected for interstellar absorption) of
HD 223460 in the 0.3-2 keV and 2-10 keV measured with
the combined EPIC MOS and pn cameras. The percentage contribution
in luminosity of hot plasmas (kT> 1 keV) is indicated between
bracketts. The hardness ratio (hr) is defined as
.
The spectral analyses of each observation were conducted
separately. Spectral fitting of the EPIC data (see Sect. 5.1) during
these two periods yields flux measurements in the 0.3-2 keV and >2
keV bands. These measurements were converted into X-ray luminosities
and
using Hipparcos parallax
(
mas; ESA 1997). The luminosities are given in Table 3
which also provides the hardness ratio hr of the X-ray emission
defined as
.
Table 3 confirms that the X-ray spectrum
of HD 223460 is soft. Compared with revolution 200, the X-ray
luminosity of HD 223460 during revolution 107 was 19% higher in the
0.3-2 keV band and about 46% higher in the >2 keV energy band.
The two EPIC datasets (see Fig. 3) were fitted separately with the MEKAL optically thin plasma emission model (Mewe et al. 1985). The spectral fitting was performed in the 0.3-9 keV and 0.3-6.5 keV spectral bands for revolutions 107 and 200, respectively since revolution 200 data does not contain any significant signal above 6.5 keV. The interstellar hydrogen column density was left free to vary.
values in the range
(3.1-
cm-2 were derived from the analysis of the two datasets which are lower than the total galactic H I column density
cm-2 (Dickey & Lockman 1990) in the direction
of HD 223460. No single temperature plasma model that assumes either
solar photospheric (Anders & Grevesse 1989) or non solar abundances
can fit the data, as unacceptably large values of
were
obtained. The MEKAL plasma models with two components at different
temperatures prove adequate for the two datasets (see Table 4). The
coronal emission measure distribution has been proposed to be
double peaked for many stars (Schrijver et al. 1995; Mewe et al. 1996;
Güdel et al. 1997a, 1997b). In particular, best fit MEKAL models to
data obtained in January 1993 (Singh et al. 1996)
suggests a coronal plasma in HD 223460 with two components at distinct
temperatures. Different models could produce acceptable fits to the
PSPC spectra, some of which with best fit temperatures
similar to those derived from EPIC data.
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Figure 3:
Best fit models to revolution 107 (left) and revolution 200 (right) EPIC spectra. The data (crosses) and spectral fit (solid line) to the EPIC pn (upper curve) and EPIC MOS (lower curve) spectra are shown in the upper panel. The ![]() |
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Table 4: Best fit parameters to EPIC data using a 2 components MEKAL model (Mewe et al. 1985) with variable abundance and a variable hydrogen column density.
Table 5: Best fit parameters to EPIC data using a 3 components MEKAL model (Mewe et al. 1985) with variable abundance and a variable hydrogen column density.
As spatially unresolved observations gain in spectral resolution and
signal to noise ratio, the amount of details in the spectra of stellar
coronae which must be reproduced increases reflecting the true
complexity of the sources plasma. Multi-temperature models are now
necessary to explain high-resolution spectra of stellar coronae
(Dupree et al. 1993; Griffiths & Jordan 1998; Bowyer et al. 2000). Recent analysis of XMM-Newton and
X-ray spectra find that a continuous emission measure distribution
fits the data better and is more realistic physically (Audard et al. 2001a,b; Güdel et al. 2001; Mewe et al. 2001). Hence, we tried
to fit the EPIC spectra of HD 223460 using a MEKAL model with three
components at different temperatures and with the same
metallicity. The improvement in
statistics compared with
the two temperatures model (
for
747 degrees of freedom and
for 539
degrees of freedoms on the best fit to revolution 107 and 200
datasets, respectively) is significant to a >99% confidence level
using the F-statistic. The "cool'' component in the three component
model has a slightly lower temperature but an emission measure similar
to that given by the two component model. The three component model
suggests that most of the emission measure of the "hot'' plasma is
located around
K but with a significant
contribution above
K. The
emission measure and temperature of this very hot plasma component are
not well constrained. The temperatures of the different plasma
components remain the same for revolution 107 and 200. Hot (
K) plasma on HD 223460 is the main source of X-ray
emission both in the soft and in the hard X-ray band. It
contributes to 98% of the X-ray luminosity above 2 keV. Table 5
shows that the higher X-ray luminosity of HD 223460 in revolution 107
both in the soft and in the hard energy range is related to a higher
emission measure of the hottest plasma. The average element abundance
in HD 223460 corona is found to be lower than the solar photospheric
value (see Tables 4 and 5). No significant variations of abundance are
detected between the two revolutions.
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Figure 4: Comparison of the EPIC pn spectrum of HD 223460 obtained during revolution 107 with a best fit power law + Gaussian model in the 3-9 keV range. |
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One major feature of HD 223460 spectrum during revolution 107 is the
presence of a high energy tail and of an emission feature around 6.6
keV attributed to an iron K emission line (see Fig. 4). This component
is not detected in revolution 200 data. The iron Kfluorescence line consists of two components K
and K
at 6.404 keV and 6.391 keV respectively for Fe I and a
branching ratio of 2:1 (Bambynek et al. 1972). The natural width of
the lines (
eV) and any broadening due to
thermal motions of the emitting atoms (
)
are negligible compared to the energy resolution
(155 eV FWHM) of the EPIC cameras. The iron K
fluorescent line
energy is an increasing function of the ionization state. It rises
slowly from 6.40 keV in Fe I to 6.45 keV in Fe XVII (neon-like) and
then increases steeply with the escalating number of vacancies in the
L-shell to 6.7 keV in Fe XXV and 6.9 keV in Fe XXVI (House 1969;
Makishima 1986). Spectral fits to the EPIC p-n spectra above 3 keV
by a powerlaw and a Gaussian line model give a power law with a slope
and an Fe K line at
keV with an
equivalent width
eV and a flux
erg cm-2 s-1. The improvement of the
power law fit with an additional Gaussian line is significant (
for 32 degrees of freedom) to a >95%
confidence level using the F-statistic. This result indicates the
presence of iron in high Fe XXV states of ionization during revolution 107. For a collisionally dominated optically thin coronal plasma, the
Fe XXV ion concentration reaches a maximum value in the 2-
K temperature range (Raymond-Smith 1977), in agreement with the
temperature of the hot plasma component derived by spectral
fitting. This supports the thermal origin of the Fe K emission.
Table 6:
Best fit parameters to RGS spectra in the 0.5-1.3 keV range
recorded in revolutions 107 (upper table) and 200 (lower table)
using a three components VMEKAL model. The temperature of each
component were frozen to the value derived from the analysis of EPIC
data (see Table 5). The metallicity was left free to vary. The
oxygen and neon abundances were first tied to the abundance of the
other elements (MODEL A). There were then left free to vary
independently but with the same value for the different temperature
components (MODEL B). In MODEL C, the hottest temperature component
has been replaced by a VMEKAL component at
K
where the Ne IX line is formed.
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Figure 5:
Comparison of the RGS spectra of HD 223460 obtained during
revolution 107 with a best fit VMEKAL model with 3 temperature
components (see Table 6, model C) in the 10-25 Å range. The
data (crosses) and spectral fit to the RGS spectra are shown in the upper panel. The ![]() |
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Among all of the different changes, eruption and instabilities which
are seen on the Sun, the ones which are labeled "flares'' all have
in common material heated to temperatures of 107 K or higher
(Golub & Pasachoff 1997; Reale et al. 2001). Such temperatures are
not seen in the non-flaring corona, and events which do not produce
such hot plasma do not seem to be called flares. The emission measure
of some active stellar coronae has two peak, one at at a few 106 K and the other around 107 K, and it has been proposed that the higher
temperature peak is due to continuous flaring activity (Drake et al. 2000; Sanz-Forcada et al. 2002). However, such a flaring activity is
expected to induce count rate fluctuations that are not observed in
the EPIC light curves of HD 223460. Hence, also suggestive, the existence of
significant amounts of 107 K material and the detection of Fe XXV
emission cannot be regarded as a proof for the presence of
flares in the corona of HD 223460.
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Figure 6: Averaged first order spectra of RGS 1 and 2 obtained during revolutions 107 (top) and 200 (bottom). |
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The low energy RGS spectra were fitted with a VMEKAL model with three
components at different temperatures. The VMEKAL model generates a
spectrum of hot diffuse gas with line emission from several elements
based on the calculation of Mewe et al. (1985) with Fe L calculations
by Liedahl (1995). Hence, three electron temperatures and electron
densities are assumed for the entire ensemble of element charge states
and in particular for iron, oxygen and neon which produce the most
prominent lines. This assumption turns out to be fairly adequate
within the observational uncertainties of the present spectrum (see
Fig. 5). The fit was performed in the spectral range from 9.5 Å to
25 Å where the efficiency of the RGS spectrometers is the
highest. The model temperatures of the cool, mid-temperature and hot
plasma components were frozen to the values derived from EPIC data
(see Table 5). The abundances of the O and Ne elements which give
prominent lines in the considered spectral range were first tied to
the abundance of the other elements (MODEL A). They were then allowed
to vary independently but with the same value for all temperature
components (MODEL B). In a third model (MODEL C), the hottest
temperature component has been replaced by a VMEKAL component at
K where the Ne IX line is formed. Fitting
results are given in Table 6. The photon statistics in the RGS spectra
of revolution 200 is lower than in the revolution 107 dataset. The fit
supports the three components plasma model for the interpretation of
the EPIC and RGS data. The emission measures of low and hot
temperature components are similar to the values derived from the
analysis of EPIC spectra (see Table 5). However, the emission
measure of the mid-temperature component in RGS is higher
(
cm-3) than the value derived from
EPIC data (
cm-3) as suggested
by the line flux measurements (see Table 7). When left free to
vary, the oxygen abundance is similar to the average abundance of the
other elements. The determination of abundances relative to hydrogen
requires an accurate measurement of the X-ray continuum which cannot
be reliably measured even from the RGS spectra (see Fig. 5) due to
their moderate spectral resolution and signal to noise
ratio. Therefore it is modeled from the flux left over when all of the
known emission lines in the VMEKAL model are included. However, no
plasma spectroscopy code includes all of the emission lines, so the
missing weak emission lines are misinterpreted as continuum flux
(Schmitt et al. 1996), thereby raising the hydrogen abundance derived
from the free-free continuum and lowering all of the metal abundances
relative to hydrogen. This systematic error in the metal abundances
relative to hydrogen is not included in the abundance uncertainties
stated in Table 6 but the fitting results suggest that neon abundance
of the hot plasma component is significantly higher than the oxygen
abundance. The improvement in
fit statistics
(
for 411 degrees of freedom and
for 221 degrees of freedom,
respectively for revolution 107 and 200) induced with variable O and
Ne abundance is significant at >99% confidence using the
F-statistic. Hence, the Ne/O ratio found for HD 223460 seems higher
than in the solar photosphere. This indication of a Ne abundance
enhancement is reminiscent of a similar anomaly observed in a subset
of solar flares (Murphy et al. 1991; Schmelz 1993). Large Ne
abundance enhancements are a common feature of active stellar coronae
(Güdel et al. 2001; Huenemoerder et al. 2001) and an inverse FIP
effect is observed in very active coronae (Brinkman et al. 2001;
Drake et al. 2001) where the abundances (relative to oxygen) increase
with increasing first ionization potential (FIP).
Figure 6 shows the RGS spectra of HD 223460 averaged over revolution 107 and 200. Each spectrum is the sum of the two spectra
simultaneously obtained with the RGS1 and RGS2 reflection grating
spectrometers on board XMM-Newton. Line fluxes and positions
were measured using the XSPEC package by fitting simultaneously the RGS1 and RGS2 spectra with a sum of narrow Gaussian emission lines
convolved with the response matrices of the RGS
instruments. The continuum emission was described using bremsstrahlung
models with temperatures frozen to the best fit values derived by spectral
fitting (see Table 6; MODEL C). The strong lines were included in the
fit, so the continuum of the weaker lines is better evaluated. For
line identification, we required only that the wavelength coincidence
be comparable to the spectral resolution of the RGS spectrometers,
namely 0.04 Å over the 5 to 35 Å wavelength range. In the X-ray
domain, several candidate lines may exist within this acceptable
wavelength coincidence range. Hence, we only looked for resonance
transitions of abundant elements, and predicted line intensities using
spectra of the Sun (Doschek & Cowan 1984) and of Capella (Brinkman et al. 2000). Series of lines of highly ionized Fe and several lines of
the Ly and He series are visible in RGS spectra, most notably from O
and Ne. Estimates or upper limits of line fluxes are reported in Table 7. Their temperatures of maximum formation range between
K and
K suggesting that the corresponding
ions are mainly associated with the cool plasma components inferred from EPIC
data. However, lines such as the O VIII and Ne X lines have emissivity
functions quite spread out in temperature to which material
present in the hot component contributes too. Also, the Ne IX line indicates
the presence of cooler material than the cool component
reported. No significant line intensity variations are observed
between revolutions 107 and 200. The Ne X (12.13 Å), Ne IX (13.45 Å) and Fe XIX (13.74 Å) lines are affected by blends. This
could explain that their flux upper limits (see Table 7) are
inconsistently high compared with the values expected from the
analysis of EPIC spectra. Lines with low temperature (
K) of maximum line formation give emission measures
consistent with the values
cm-3 and Z = 0.2 of the EPIC low temperature plasma component
(see Table 5). The Fe XVIII (14.56 Å) and Fe XXII (11.79 Å) lines
whose temperature of maximum formation is greater than
K give emission measures higher than the value
cm-3 of the EPIC mid-temperature plasma
component (see Table 5). This is likely due to uncertainties in
their flux determination although effects related to the
cross-calibration accuracy between EPIC and RGS are not excluded.
The emitting volume of the different plasma components could be constrained if their electron densities were known. These can be measured using density-sensitive spectral lines originating from meta-stable levels, such as the forbidden (f) 23S-11S line in helium-like ions. This line and the associated resonance (r) 21P-11S and inter-combination (i) 23P-11S lines make up the so-called helium-like triplet lines (Gabriel & Jordan 1969; Pradhan 1982). The intensity ratio (i+f)/r varies with electron temperature and the ratio i/f varies with electron density due to the collisional coupling between the meta-stable 23S upper level of the forbidden line and the 23P upper level of the inter-combination line. The RGS wavelength band contains the He-like triplets from O VII, Ne IX, Mg XI and Si XIII. However, the Si, Mg and O triplets are not detected in the RGS spectra of HD 223460 and the Ne IX triplet is too heavily blended with iron and nickel lines for density analysis.
Table 7: Measured positions and flux estimate or upper limits of the strongest lines in the RGS spectra of HD 223460 obtained during revolutions 107 and 200. The columns give the predicted line positions, the measured line positions during revolution 107, the measured line positions during revolution 200, the ion and line identifications, the temperatures of maximum line formation, the line fluxes measured during revolution 107 and the line fluxes measured during revolution 200.
The spectral fitting of the EPIC and RGS spectra of HD 223460 suggests
a corona configuration with little contribution from quiet regions
similar to the Sun. On the contrary the temperature
K of the "cool'' plasma component is reminiscent of
solar type active regions, while the hot (
T > 107 K) component
may be caused by disruptions of magnetic fields associated to a
permanent flaring activity. The review of coronal activity by Vaiana
& Rosner (1978) pointed out that the Sun, if completely covered with
active regions, would have an X-ray luminosity of
ergs s-1. When scaled to the surface of HD 223460 (
-13
;
see Table 1), an X-ray luminosity of about (2.0-3.4)
erg s-1 is obtained. This value is comparable
with the observed X-ray luminosity of HD 223460 ((3-4)
erg s-1) derived using Hipparcos parallaxes. It is
higher than the X-ray luminosity contribution (
(5.1-6.2)
erg s-1) of its "cool'' (
K) plasma component. The X-ray luminosity of the
"cool'' plasma component could be explained if 15-31
of the
surface of HD 223460 is covered with bright solar like active
regions. Assuming that these active regions can be described by a
simple static loop system consisting of similar loops of constant
pressure p (dyn cm-2), temperature T (K) and cross section A (cm2), the emission measure EM (cm-3) of the "cool''
plasma can be expressed as:
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(1) |
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(2) |
Table 8:
Physical parameters of HD 223460 coronal loops derived from
the XMM-Newton observations conducted during revolution 107
and 200. The electron density is derived from Eq. (1), i.e.
.
If, in HD 223460, the cool plasma components is produced by solar like
active regions covering a large fraction of the star's surface, it is
easy to imagine that such a dense population of active regions
coexists with constant interaction and disruption of their magnetic
fields which might be expected to lead to continuous flaring. This
could explain the permanent emission measure of hot plasma above 107 K. High temperature plasmas have been detected from the Sun
and from non-solar coronae (van den Oord & Mewe 1989; Tsuru et al. 1989). The
solar flare plasma shows a bimodal temperature distribution with
plasma at two different temperature (4-
K and
(16-
K where the hot component is present only
during the flares (Antonucci & Dodero 1995). The two components
probably have a common origin in the flaring region on the Sun. It is
worth noting that the temperature of these components are close to the
plasma temperatures derived from the spectral analysis of HD 223460
X-ray emission. There is evidence that the emission measure
distribution of very active stellar coronae, obtained from spectrally
resolved XUV observations, is double-peaked. A study of the transition
regions and coronae of the RS CVn binaries V711 Tau, AR Lac and II Peg
(Griffiths & Jordan 1998) indicates the existence of two distinct
peaks in the high temperature emission measure distribution around
K and
K. Recently, Sanz-Forcada
et al. (2002) derived the emission measure distribution of a sample of
RSCVn binaries and single active stars including the low-rotation
giant
Cet. They noticed that emission measure distributions are
remarkably similar among all the stars, showing a narrow enhancement
or bump around
.
This aspect is much
debated and still open, but it has been suggested that this hot
component may be due to a continuous flaring activity (Güdel 1997;
Drake et al. 2000). The surface of active stars is covered by active
regions, and flares would be so frequent that their light curves
overlap, canceling out any variability due to single events. Reale et al. (2001) showed that a double-peaked emission measure distribution
is obtained if one combines the EM(T) of the whole solar corona with
the envelope of the EM(T) profiles during solar flares. This seems
to suggest that uninterrupted sequence of overlapping proper flares,
whichever their evolution, could produce a double peak emission
measure distribution in the coronae of active stars. This could
explain the presence of hot coronal material even in the absence of
obvious flares. There could be small-scale flares not well identified
in the light curve of XUV data with moderate signal-to-noise ratio. Within this interpretation, the higher emission measure and
luminosity contribution of the hot plasma component in revolution 107
would be related to a more intense flaring activity of HD 223460 in
July 2001. On the other hand, the steady flux decrease during
revolution 107 and flux increase during revolution 200 could be
interpreted as the gradual disappearance or emergence of active
regions at the limb of the star. Since active regions might not be
homogeneously distributed on the surface of the star, it is difficult
with the presented data to distinguish between a long-term variability
of the flaring activity and a rotational modulation of the X-ray
emission by long lived active regions.
One hypothesis regarding HD 223460 origin (see Sect. 2) is that the
star originates from a single, early B-type star as it evolves in the
giant domain, crosses the Hertzsprung gap and becomes a convective
late-type giant. To be likely, this scenario should account for the
photometric period of the star (
days;
Strassmeier & Hall 1988) and for the recent estimate (
25 km s-1; see Table 1) of its equatorial velocity. We
compared this value with
values of A-F giants extracted
from the Bright Star Catalogue and with
measurements of G-K
giants obtained with CORAVEL by de Medeiros & Mayor (1995). The
CORAVEL measurements are precise to about 1 km s-1. All projected
equatorial velocity measurements are plotted in Fig. 7 as a function
of
for different mass ranges. A-F giants (
K) have high rotational velocities, often greater than 100 km s-1. K giants, on the contrary, have low
values of 1 or 2 km s-1 for
K. As noticed by Simon &
Drake (1989), stellar rotation strongly decline during the rapid
evolution of G giants across the Hertzsprung gap. These authors also
suggested, along with Gray (1989), that magneto-hydrodynamic braking
due to stellar winds could explain this phenomenon. Rutten & Pylyser
(1988) argued that during the entire evolution of a 3
star
the timescale for magnetic braking is larger than the evolutionary
time scale. Endal & Sofia (1979) and Gray & Endal (1982) pointed out
that the expansion of the stars on the red giant branch together with
the rearrangement of angular momentum due to the increasing depth of
the convection zones may well explain the decrease of
for
cool giants. Gondoin et al. (2002) calculated the equatorial velocity
evolution of 2.5
giants using Schaller et al. (1992)
evolutionary models and assuming angular momentum conservation and
km s-1 at
K. Comparisons with
measurements (see Fig. 7) confirm that angular momentum
conservation alone cannot explain the rotational velocities of K giants. However, Fig. 7 suggests that HD 223460, which is located near
the bottom of the RGB, just starts experiencing rotational
braking. Most of its angular momentum could have been conserved within
its convective envelope during its rapid evolution from mid-F spectral
type. Evolution from an early B type star with a moderate rotation
velocity could then explain the current rotation period of the star.
![]() |
Figure 7:
Equatorial rotational velocity of HD 223460 (filled circle) compared with ![]() ![]() ![]() ![]() ![]() |
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![]() |
Figure 8:
XMM-Newton luminosities of HD 223460 (filled circles)
in the 0.3 to 2 keV band compared with ROSAT PSPC measurements of
single field giants (Hünsch et al. 1998; Pizzolato et al. 2000). Upper limits of X-ray luminosities measured with the
Einstein (Maggio et al. 1990) and ROSAT (Pizzolato et al. 2000)
observatories are indicated by small triangles, large triangles and
filled triangles for low-mass (1.2
![]() ![]() ![]() |
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Within this hypothesis, the outer convection zone of HD 223460 would
have deepened since its formation at mid-F spectral type, thus
increasing the convective turnover time scale (Gilliland 1985). Since
HD 223460 only experienced a small spin down (see Fig. 7) and
maintained a relatively high rotation rate, the Rossby number (Durney
& Latour 1978) decreased and dynamo activity increased as the star
evolved towards the bottom of the RGB. During this period, the
deepening convective envelope likely suffered shear stresses, which
could have resulted in radial velocity gradients. The necessary
conditions were then present to switch on an -
dynamo
with an increasing efficiency as the star evolved towards the bottom
of the RGB. Our spectral analysis of the X-ray data suggests that the
fluid kinetic helicity induced by the rotation currently generates
magnetic fields with characteristic scale of 1010 cm, i.e.
comparable with large interconnecting solar loops. The dynamo
productive of large magnetic flux induces a high density of active
regions covering up to 30% of the star surface. We argue that the
X-ray emission is strongly enhanced due not only to the occurrence of
these large scale magnetic structures, but also to their permanent
interactions. These interactions would lead to an uninterrupted flaring
activity that generates a large volume of hot plasmas. Since HD 223460
could be soon ascending the RGB, it is anticipated that its rotation will
spin down dramatically with the effect of increasing its Rossby number
and decreasing its helicity-related dynamo-driven activity. Not only
the rotational braking per se but also the restoration of rigid
rotation could prevent the maintenance of large magnetic structures as
the star ascends the red giant branch (Gondoin 1999). Rosner et al. (1995) pointed out that this suppression of a large-scale dynamo
leads to the disappearance of large-scale organized stellar magnetic
fields but does not imply the suppression of magnetic field production
at small scale, driven by the turbulent motion in the surface
convection zones. A bifurcation in magnetic loop sizes could occur as
the dynamo induced by rotation gives way to a turbulent field
generation mechanism like that described by Durney et al. (1993). According to this scenario, X-ray emission from large
coronal loops and the related flaring activity should progressively
disappear as HD 223460 evolves from G to K spectral type (see Fig. 8).
![]() |
Figure 9: Ratio of the X-ray to bolometric luminosities of HD 223460 (filled circles) in the 0.3 to 2 keV band compared with single field giants (Hünsch et al. 1998; Gondoin 1999; Pizzolato et al. 2000). |
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The above evolution scenario implies that, from the successive effects
of convection zone deepening and rotational braking, a minimum value
of the Rossby number is expected around HD 223460 evolutionary
stage. At this stage,
dynamo mechanisms (Parker 1955)
should operate with maximum efficiency. Capella observations
(Johnson et al. 2000) of the Fe XXI
1354 formed at 107 K
suggest a significant variability over the past 5 years in the hottest
part of the corona of the G8 III primary thought to be a He-burning
clump giant. This suggests that cyclic activity and strong variability
are seen in late evolutionary stages. The positive effect of deepening
convective envelope on coronal activity would allow even the slowly
rotating new arrivals to the clump still to be somewhat active (Ayres
et al. 1998). We compared our X-ray flux measurements of HD 223460
(see Sect. 4) in the 0.3 to 2 keV band with X-ray fluxes of single
field giants extracted from the ROSAT all-sky survey catalogue
(Hünsch et al. 1998). Upper limits of Einstein X-ray fluxes
were also retrieved from Maggio et al. (1990). We calculated the X-ray
luminosities (
)
of all stars from the Hipparcos
parallaxes. The results are presented in Fig. 8 as a function of
for different mass ranges. X-ray luminosities of single
giants recently derived from ROSAT data (Pizzolato et al. 2000) are
also included. The X-ray emission of giants reaches a maximum value in
the effective temperature range
K
corresponding to G spectral types. Figure 8 confirms that the X-ray
luminosity of HD 223460 is among the highest within this sample of
single nearby F, G and K giants, thus supporting the above evolution
scenario. Figure 9 shows that the X-ray-to-bolometric luminosity ratio
of HD 223460 is also one of the highest. This indicates that the high
X-ray luminosity of HD 223460 results from an increased density
of active regions related to its evolutionary position rather than from its
large emitting surface. The coronal structure and evolutionary status
of HD 223460 would thus be similar to that of FK Comae (Gondoin et al. 2002) and V390 Aurigae (Gondoin 2003). This justifies the
classification of HD 223460 as an FK Comae-type star (Fekel &
Marshall 1991). These stars seem to be normal 2-3
giants
with A or B type progenitors on the main sequence that are evolving
near the bottom of the red giant branch.
The analysis of HD 223460 data suggests that its corona is dominated
by the same type of active regions as on the Sun. However, the surface
area coverage of these active regions may approach up to 30% and
the size of the associated magnetic structures can be similar or
larger than that of interconnecting loops between solar active regions
while their temperature is hotter. One hypothesis is that the
interaction of these structures themselves induces a flaring activity
on a small scale not visible in the EPIC light curves that
is responsible for heating HD 223460 plasma to coronal temperatures of
K. The H-R diagram position of HD 223460 suggests that
its rotation will spin down in the future with the effect of
decreasing its helicity-related, dynamo-driven activity and
suppressing large scale magnetic structures in its corona. The coronal
structure and evolutionary status of HD 223460 are thus similar to that
of FK Comae.
Acknowledgements
I thank my colleagues from the XMM-Newton Science Operation Center for their support in implementing the observations. I am grateful to the anonymous referee for the helpful comments that allowed to improve the paper.