Seismic analysis of 70 Ophiuchi A: A new quantity proposed
The basic intent of this paper is to model 70 Ophiuchi A using the latest asteroseismic observations as complementary constraints and to determine the fundamental parameters of the star. Additionally, we propose a new quantity to lift the degeneracy between the initial chemical composition and stellar age. Using the Yale stellar evolution code (YREC7), we construct a series of stellar evolutionary tracks for the mass range = 0.85 – 0.93 with different composition (0.26 – 0.30) and (0.017 – 0.023). Along these tracks, we select a grid of stellar model candidates that fall within the error box in the HR diagram to calculate the theoretical frequencies, the large- and small- frequency separations using the Guenther’s stellar pulsation code. Following the asymptotic formula of stellar -modes, we define a quantity which is correlated with stellar age. Also, we test it by theoretical adiabatic frequencies of many models. Many detailed models of 70 Ophiuchi A have been listed in Table 3. By combining all non-asteroseismic observations available for 70 Ophiuchi A with these seismological data, we think that Model 60, Model 125 and Model 126, listed in Table 3, are the optimum models presently. Meanwhile, we predict that the radius of this star is about 0.860 – 0.865 and the age is about 6.8 – 7.0 Gyr with mass 0.89 – 0.90 . Additionally, we prove that the new quantity can be a useful indicator of stellar age.
keywords:Stars: oscillations; Stars: evolution; Stars: individual: 70 Ophiuchi A
The solar five-minute oscillations have led to a wealth of
information about the internal structure of the Sun. These results
stimulated various attempts to detect solar-like oscillations for a
handful of solar-type stars. Individual -mode frequencies have
been identified for a few stars: Cen A (Bouchy and Carrier,
2002; Bedding et al., 2004), Cen B (Carrier and Bourban,
2003a; Kjeldsen et al., 2005), Arae (Bouchy et al., 2005), HD
49933 (Mosser et al., 2005), Vir (Martić et al., 2004a;
Carrier et al., 2005b), Procyon A (Martić et al., 2004b;
Eggenberger et al., 2004a), Bootis (Kjeldsen et al., 2003;
Carrier et al., 2005a), Hyi (Bedding et al., 2001; Carrier
et al., 2001) and Eri (Carrier et al., 2003b). Based on
these asteroseismic data, numerous theoretical analyses have been
performed in order to determine precise global stellar parameters
and to test the various complicating physical effects on the stellar
structure and evolutionary theory (Thévenin et al., 2002;
Eggenberger et al., 2004b, 2005; Kervella et al., 2004; Miglio and
Montalbán, 2005; Provost et al., 2004, 2006).
Recently, Carrier and Eggenberger (2006) detected solar-like oscillations on the K0 V star 70 Ophiuchi A (HD 165341), and identified some possible existing frequencies. They obtained the large separation by observation over 6 nights with HARPS. The spectroscopic visual binary system 70 Ophiuchi is one of our nearest neighbors (5 pc) and is among the first discovered binary stars. It was observed first by Herschel in 1779. So 70 Ophiuchi A is famous as the primary of a visual and spectroscopic binary system in the solar neighborhood. Although many observation data have been obtained since 1779, the theoretical analysis of 70 Ophiuchi A has only been made by Fernandes et al. (1998). By a calibration method which take into account the simultaneous evolution of the two members of the binary system, they analyzed the 70 Ophiuchi A by means of standard evolutionary stellar models using the CESAM code bf (Morel, 1997) without microscopic diffusion. They found that the metallicity of 70 Ophiuchi A is very close to the solar one, the values of mixing-length parameter and helium abundance Y are near the Sun. They thought that the star is younger than the Sun and Gyr is probably an limit considering the age versus stellar rotation relation with its rotation velocity ( ).
The aim of our paper is to present the model which can be constrained by these seismology data. The observational constraints available for 70 Ophiuchi A are summarized in Sect. 2, while the numerical calculations are presented in Sect. 3. The seismic analyses are carried out and a new quantity as a indication of stellar age is proposed in Sect. 4. Finally, the discussion and conclusions are given in Sect. 5.
2 Observational Constraints
2.1 Non-asteroseismic observation constraints
|Effective temperature (K)||(2)|
|Surface heavy element abundance||(3)|
References.—(1) Fernandes et al. (1998), (2) Gray and Johnson (1991), (3) this paper.
The mass of this star was investigated by Batten et al. (1984), Heintz et al. (1988), Fernandes et al. (1998) and Pourbaix et al. (2000), respectively. In the paper, we adopt the value of mass deduced from Fernandes et al. (1998). The effective temperature was determined by Gray and Johnson (1991). So far, the metallicity obtained by observation are [Fe/H] = -0.05 (Peterson, 1978) and [Fe/H] = 0.00 (Perrin et al., 1975). We choose the [Fe/H] = 0.0 0.1 as a representative value according to Fernandes et al. (1998).
The mass fraction of heavy elements, , was derived assuming and (Grevesse and Sauval, 1998), for the solar mixture. So we can deduce the = 0.0183 – 0.0290.
All non-asteroseismic observational constraints are listed in Table 1.
2.2 Asteroseismic constraints
Solar-like oscillations of 70 Ophiuchi A have been detected by Carrier and Eggenberger (2006) with the HARPS spectrograph. Fourteen individual modes are identified with amplitudes in the range 11 to 14 . Although they listed two groups of frequencies by mode identification (see Table 2 in Carrier and Eggenberger, 2006), one group of frequencies with a average large separation was suggested to be more reliable than the other with a average large separation . The star 70 Ophiuchi A is very similar to Cen B with the same spectral type and similar large separation, which has a mean small separation of 10 . It is thought that the small separation should be similar. By inspecting the results of the mode identification, they note that the value of the small separation coming from the identification with the large separation of 172.2 is significantly different from 10 . If the large separation is 172.2 , the small separation will be lower than 6.5 in the frequency range 3 – 4.5 . Although this identification is less reliable than the one with a large separation of 161.7 , the solution = 172.2 can not be ruled out definitely. We refer to these two groups of results in the paper and make analyses in Sect. 4 and Sect. 5.
3 Stellar models
|Variable||Minimum Value||Maximum Value|
|Initial heavy element abundance||0.017||0.023||0.001|
|Initial Helium abundance||0.30||0.01|
Note.—The value defines the increment between minimum and maximum parameter values used to create the model array.
We will construct a grid of stellar evolutionary models by Yale stellar evolution code (YREC; Guenther et al., 1992) with microscopic diffusion. The initial zero-age main sequence (ZAMS) model used for 70 Ophiuchi A was created from pre-main sequence evolution calculations. In these computations, we do not consider rotation and magnetic field effect. These models are computed using OPAL equation of state tables EOS2001 (Rogers and Nayfonov, 2002), the opacities interpolated between OPAL GN93 (Iglesias and Rogers, 1996) and low temperature tables (Alexander and Ferguson, 1994). Using the standard mixing-length theory, we set for all models, close to the value which is required to reproduce the solar radius under the same physical assumptions and stellar evolution code. Meanwhile, it must be emphasized that there are still a number of uncertainties in our analyses, foremost among which is the still open question of mixing-length theory responsible for the stellar model. The nuclear reaction rates have been updated according to Bahcall and Pinsonneault (1995). The Krishna-Swamy Atmosphere T- relation is used for this solar-like star (Guenther and Demarque, 2000). Also, we consider the microscopic diffusion effect, by using the diffusion coefficients of Thoul et al. (1994). Since 70 Ophiuchi A, like Cen B, is less massive than the Sun, the mass contained in its convective zone is much larger and, therefore, the effect of microscopic diffusion is much smaller (Miglio and Montalbán, 2005; Morel and Baglin, 1999). However, it is necessary to consider this effect as physical process in stellar modeling (see Provost et al., 2005, 2006).
In general, the determination of parameters fitting the observational constraints needs two steps. The first step is to construct a grid of models with position in the HR diagram in agreement with the observational values of the luminosity, the effective temperature and the surface metallicity. The principal constraints deduced from non-asteroseismic observation are listed in Table 1. The error box, which is composed of observational effective temperature and luminosity, represents the possible position of 70 Ophiuchi A in the HR diagram (see Fig. 1a). According to the results of Fernandes et al. (1998), we list the parameter space of mass M, the initial heavy-element abundance and the initial helium abundance in Table 2. Since the microscopic diffusion is included in our paper, we give the wider parameter space of initial heavy-element abundance than the range of of Fernandes et al. (1998).
By adjusting three parameters , and listed in Table 2, we can obtain many evolutionary tracks passing through the error box in the HR diagram. Now we consider a function which describes the agreement between the observations and the theoretical results:
where represent the following quantities: , and , represent the theoretical values and represent the observational values listed in Table 1. The vector contains the errors on these observations which are also given in Table 1.
As Fernandes(1998) has pointed that the age of 70 Ophiuchi A is Gyr, it is reasonable for us to choose the evolutionary tracks passing through the error box within 8 Gyr. We select 44 evolutionary tracks passing through error box as our possible candidates to go on with our investigations. Fig. 1a gives 44 evolutionary tracks, and Fig. 1b presents as a function of the age correspondingly. It is well-known that is smaller, the more competitive is the candidate. Fig. 1b shows that models with smaller than 1 have ages between 3Gyr to 7Gyr. From Fig. 1a, we find that the upper section of error box is empty. The reason of the empty upper section of the error box is related to the range of initial parameters, like mass, initial composition and specially the mixing length parameter. We think that the future interferometric measurement of the radius could reduce the domain of the possible position in the HR diagram (e.g., Provost et al., 2006).
The second step is to determine the optimum model using the asteroseismic measurements. We will select a grid of models along these 44 tracks shown in Fig. 1a to calculate the low- -modes frequencies. We list the representative models extracted from every tracks in Table 3.
The detailed pulsation analysis is described in the next section.
4 Pulsation analysis
4.1 Selecting the optimum model
Using Guenther’s pulsation code (Guenther, 1994), we calculate the adiabatic low- -mode frequencies of the selected models. We define the large separations and small separations in the usual way (Tassoul, 1980):
where is the radial order, is the degree, and is the frequency. Because the expected acoustic cutoff has a limit, we only calculate the mean large- and small- separations by averaging over = 10 – 30 (See Murphy et al., 2004). Within these 44 tracks, we list 129 models in Table 3. represents the mean of large separations for = 10 to 30. The frequency range corresponds to about 2000 –6000 . Additionally, represents the mean of for to 3. In the same way, and represent the mean of and for = 10 to 30, respectively. So far, we only know the large separations and the fourteen individual modes of the star based on the asteroseismic data of Carrier and Eggenberger (2006). Guenther (1998) pointed that the large separations are most easily identifiable characteristics in the -mode spectrum. Because they are seen as a peak in the Fourier transform of the power spectrum and they are mostly uncontaminated by composition effects, these large separations provide an efficient way to constrain stellar model. It is also important to remember that the theoretical frequencies calculated in our paper should not be expected to match the observed frequencies of Carrier and Eggenberger (2006) perfectly. We think that there are three reasons. Firstly, our theoretical models do not match the mass and radius of the star precisely. Secondly, the uncertainty in calculating the sound speed in the outer layers of the models comes into being, where non-adiabatic effects become important. Thirdly, at high frequencies, the effect of the convection-oscillation interactions is larger and the description of convection is open problem. Although the differences between the theoretical frequencies and the observed frequencies could result in significant effect on the large separations, we think that the effect is small due to the large separations correspond to differences between frequencies of modes with the same angular degree and consecutive radial order . Therefore, in our paper, we think that the matching the observable large separations is the important criterion to select the optimum model. In Table 3, we find that the average large separations of Model 60, Model 125 and Model 126 are 161.7, 161.92 and 161.68 , in good agreement with the mean value derived from Carrier and Eggenberger (2006). So we can tentatively say that these models may be the best fit models. In Fig. 2, we plot the observational results about the large separations and the errors. Also we plot the large separation as a function of frequency for Model 54 in Fig. 2a, Model 60 in Fig. 2b, Model 125 in Fig. 2c and Model 126 in Fig. 2d. We clearly find that the theoretical large separations of the Model 60, Model 125 and Model 126 are consistent with the observations. Model 54, as the representative of many non-fit models, is not consistent with the observational large separations. Therefore, we have sufficient reasons to say that Model 60 , Model 125 and Model 126 are really the best fit models. Meanwhile, we can predict that the radius of star is 0.860 – 0.865 and the age is about 6.8 – 7.0 Gyr with mass 0.89 – 0.90 presently.
Once the asteroseismic observation can confirm the large separations to be and the theory Model 60 , Model 125, Model 126 are considered as the best models, we can predict that the mean small separation is about 10.29 – 10.48 and the radius of the star is about 0.860 – 0.865 . Direct measurements of stellar diameters from interferometric observations should provide an independent check for asteroseismic predictions such as Kervella et al. (2003a, 2003b).
In order to compare the theoretical -mode frequencies deduced from the models in Table 3 with the observational frequencies provided by Carrier and Eggenber (2006), we plot the echelle diagram of every model and find that no model can fit observational frequencies. For the exact values of the frequencies, considering above three reasons, a linear shift of a few between theoretical and observational frequencies is perfectly acceptable. Taking into account it, we define the mean value of the difference between the theoretical and observational frequencies (e.g., Eggenberger et al., 2004b, 2005):
where is the number of observable frequencies ( = 14).
Takeing into account the systematic difference between theoretical and observable frequencies, we plot the differences between calculated and observed frequencies in Fig. 3 and the echelle diagram in Fig. 4. The observable frequencies correspond to the average large separation of 161.7 in these figures. Fig. 3a, Fig. 3b, Fig. 3c and Fig. 3d correspond to the Model 54 with , Model 60 with , Model 125 with , and Model 126 with , respectively. Fig. 4a, Fig. 4b, Fig. 4c and Fig. 4d show the echelle diagram of the Model 54, Model 60, Model 125 and Model 126 respectively. For -modes in the asymptotic theory (), the large separations are nearly constant; meanwhile the so-called “echelle diagrams” present the frequencies in ordinates, and the same frequencies modulo the average large separation in abscissa. So the asymptotic theory predicts an approximated vertical line for given degree. In this case, Fig. 4b, Fig. 4c and Fig. 4d show that the theoretical frequencies of Model 60, Model 125, Model 126 can fit the observable frequencies with 161.7 . Meanwhile, we find that the systematic differences are larger than the results of Cen B obtained by Eggenberger (2004b). It is interesting to analyze the difference in future work.
4.2 Asymptotic formula and frequency analysis
4.2.1 Large Separations and Small Separations
It is well known from asymptotic theory that the large separations are mainly sensitive to the stellar radius (Tassoul, 1980; Christensen-Dalsgaard, 1984). More precisely, the asymptotic behavior of is expected to scale with , where is the mass of the star and is its radius. Meanwhile, Murphy et al. (2004) find that a degeneracy in predicted radius occurs for models of different mass. Here, the degeneracy means that the changes with radius and mass (see Fig. 4 in Murphy et al., 2004). In order to lift the degeneracy, Fernandes and Monteiro (2003) and Murphy et al. (2004) assumed homology to compare theoretical models by introducing a “reduced” radius, such as
Here, we name the quantity “reduced” large separation. We draw the “reduced” large separation versus mass in Fig. 5 and list the values of for each model in Table 3. From Fig. 5, we find that the degeneracy was lifted approximately. It is easily seen that the values of the are relatively consistent with each mass. It is successful using the instead of large separations to indicate the stellar mass.
The small separations, like the large separations , will be visible as peaks in the Fourier transform of the power spectrum. At the earlier stage, Christensen-Dalsgaard (1984) proposed that the calculation of small separations could put a constraint on the age the star. Subsequently, Ulrich (1986) realized that only if the composition of the star is known completely can one use the small separations to correctly identify a stellar age. This point has been illustrated in Murphy et al. (2004). Thus, the various chemical compositions create a degeneracy in age determination (see Murphy et al., 2004). Namely, the small separations change with the initial composition and age. In the next section, we will discuss this problem and propose a quantity which may be correlated with stellar age.
4.2.2 A new quantity be proposed
At the present time, we can know the stellar internal structure and understand the stellar evolution from oscillation frequencies. Thus asteroseismology provides a window to “see” the interior of star. But the observation of solar-like oscillation is very difficult because of their small amplitude. So far, we only obtain the knowledge of the stellar interior from the limited modes () which can be observed. Many authors proposed some quantity as diagnostic purposes to probe the stellar internal and constraint the model parameters (Christensen-Dalsgaard, 1984, 1988, 1993; Ulrich, 1986, 1988; Gough, 1987, 1990a, 2003). For -modes of solar-like stars, the usual frequency separations are the large separation defined by equation (2) and the small separation defined by equation (3). Additionally, Roxburgh (1993) and Roxburgh and Vorontsov (2003) considered the following separations:
and defined the ratios of small to large separations as follows:
The ratios of small to large separations are independent of the structure of the outer layers of a star, and therefore provide a diagnostic of the stellar interior alone.
In addition, Gough (1990a), Monteiro and Thompson (1998), Vauclair and Théado (2004), Houdek and Gough (2007a) gave the second differences :
The second differences can be used to reveal the variation of the first adiabatic exponent dependent of the influence of the ionization of helium on the low-degree acoustic oscillation frequencies in model of solar-type stars. Recently, Houdek and Gough (2007b) stated that the second differences can provide a measure of helium abundance and hence precisely lift the degeneracy between composition and age.
Summarizing the above character separation, we find that investigation of lifting the degeneracy between the chemical compositions and the age is interesting. We begin with our investigation from a well-known asymptotic formula.
The asymptotic formula for the frequency of a stellar -mode of order and degree was given by Tassoul (1980):
where, the characteristic is related to the run of sound travel time across the stellar diameter; is a measure of the sound-speed gradient and most sensitive to conditions in the stellar core (see Gough and Novotny, 1990b; Gough, 2003; Christensen-Dalsgaard, 1993; Guenther and Brown, 2004), and are constants which are the functions of the equilibrium model. It should be noted that the classical asymptotic theory of Tassoul (1980), although providing good results at the first order in frequency, does not represent with accuracy the -mode spectrum of the stars considered. Several authors (e.g., Gabriel, 1989; Audard and Provost, 1994; Roxburgh and Vorontsov, 2000a, 2000b, 2001) have been discussed the difficulties of the asymptotic theory, particularly for evolved models with rapid variation in the sound speed in the core.
Using the equation (2) and the asymptotic formula (10), the large separation can be written as follows (Gough and Novotny, 1990b):
Taking the first order of for the approximately, we can obtain the result like Gough and Novotny (1990b) and equation (11) becomes:,
Using the same approximate method, we can obtain the expression of small separation:
Due to the small separations are rather sensitive to composition and therefore to the structure of the core, especially the extreme sensitivity of the stellar core density stratification to several parameters (Guenther and Demarque, 2000; Morel et al., 2000), we define another quantity about the ratio of average small separation adjacent in :
Using the equation (14), we calculate the values of and list it in table 3. Based on the results of numerical calculations, we plot the ratio versus age in Fig. 6. Fortunately, we find that the ratio is tightly correlated with age and decreases monotonously with age. We think that the likely reason comes from the perturbation to the gravitational potential, neglected in the asymptotic relation (10), which affects modes of the lowest degrees most strongly and which probably increases with evolution due to the increasing central density. These effects are most important for modes of the lowest degrees which penetrate most deeply and hence affect more than , leading to the dependence of on age.
From the Fig. 6, the values of in table 3 and the above discussion, we can conclude that this quantity can lift the degeneracy between the chemical compositions and age. The analysis was inspired by Fernandes and Monteiro (2003) and Murphy et al. (2004). So, we can obtain the which may indicate stellar age, if we consider a frequency ratio. As illustrated in Fig. 6, the quantity is tightly correlate with stellar age over a substantial range of the remaining parameters, including composition. At the same time, we need to point out that the range of variation of this quantity is relatively modest, compared to likely observational errors. Also, it is clear that the present data for 70 Ophiuchi A are not adequate to evaluate this quantity. We think that using this quantity to evaluate the stellar age will be convenient based on asteroseismic data which will be provided in the future.
5 Discussion and conclusions
The models of 70 Ophiuchi A are obtained by fitting effective temperature, luminosity, surface metallicity and asteroseismic observations.
We list a series of possible models in Table 3. So far, we think that Model 60, Model 125 and Model 126 are the best models. With the advance in observation, the precise asteroseismic data will provide more strict constraints on theoretical models. The conclusions of the paper are:
1. Using the latest asteroseismic observation, we try our best to construct the best model of 70 Ophiuchi A. So far, we only select the Model 60, Model 125 and Model 126, which can be fit for the observation, as the optimum models. These models are correspond to the radius of this star is about 0.860 – 0.865 and the age is about 6.8 – 7.0 Gyr with mass 0.89 – 0.90 .
2. By calculating many theoretical models, we want to use the theoretical frequencies to compare with observational frequencies and help to definitely validate the observational data.
3. We obtain a new quantity which can lift the degeneracy between the initial compositions and the stellar age. By calculation, we prove that it can be valuable for the indication of the stellar age.
4. Important point is that we test our stellar structure and evolution theory. Meanwhile we find the confrontation of observations and theoretical models. Actually we have neglect some important effects, such as rotation and magnetic field, which can impact on the internal structure and evolution. Thus, the theory models which we have constructed can not fit observation perfectly. The detailed comparisons of individual mode frequencies will also require taking into account the effects of turbulence in the outer convective unstable layers in the stellar models, which shift the observed frequencies. The parameterization of turbulence tested on the Sun by Li et al. (2002) can be applied to models for solar-like stars as well. This parameterization can be extended to other stars by using the three-dimensional radiative hydrodynamic simulations of Robinson et al. (2003), which are based on the same microscopic physics and can readily be parameterized in the YREC stellar evolution code.
We are grateful to anonymous referees for their constructive suggestions and valuable remarks to improve the manuscript. This work was supported by The Ministry of Science and Technology of the People’s republic of China through grant 2007CB815406, and by NSFC grants 10173021, 10433030, 10773003, and 10778601.
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Note.—The above mean large separations were calculated averaging over n=10, 11, 22, …, 30. The mean small separations were averages over n=10, 11, 12, …, 30 at a fixed (as indicated).