Issue 
A&A
Volume 613, May 2018



Article Number  A24  
Number of page(s)  12  
Section  Stellar atmospheres  
DOI  https://doi.org/10.1051/00046361/201732447  
Published online  25 May 2018 
Using the CIFIST grid of CO^{5}BOLD 3D model atmospheres to study the effects of stellar granulation on photometric colours
II. The role of convection across the H–R diagram
^{1}
Institute of Theoretical Physics and Astronomy, Vilnius University,
A. Goštauto 12,
Vilnius
01108,
Lithuania
email: arunas.kucinskas@tfai.vu.lt
^{2}
ZAH Landessternwarte Königstuhl,
69117
Heidelberg,
Germany
^{3}
GEPI, Observatoire de Paris, PSL Research University, CNRS, Place Jules Janssen,
92195
Meudon,
France
^{4}
LeibnizInstitut für Astrophysik Potsdam,
An der Sternwarte 16,
14482
Potsdam,
Germany
Received:
11
December
2017
Accepted:
10
January
2018
Aims. We studied the influence of convection on the spectral energy distributions (SEDs), photometric magnitudes, and colour indices of different types of stars across the H–R diagram.
Methods. The 3D hydrodynamical CO^{5}BOLD, averaged ⟨3D⟩, and 1D hydrostatic LHD model atmospheres were used to compute SEDs of stars on the main sequence (MS), main sequence turnoff (TO), subgiant branch (SGB), and red giant branch (RGB), in each case at two different effective temperatures and two metallicities, [M∕H] = 0.0 and − 2.0. Using the obtained SEDs, we calculated photometric magnitudes and colour indices in the broadband JohnsonCousins UBVRI and 2MASS JHK_{s}, and the mediumband Strömgren uvby photometric systems.
Results. The 3D–1D differences in photometric magnitudes and colour indices are small in both photometric systems and typically do not exceed ± 0.03 mag. Only in the case of the coolest giants located on the upper RGB are the differences in the U and u bands able reach ≈−0.2 mag at [M∕H] = 0.0 and ≈−0.1 mag at [M∕H] = −2.0. Generally, the 3D–1D differences are largest in the blueUV part of the spectrum and decrease towards longer wavelengths. They are also sensitive to the effective temperature and are significantly smaller in hotter stars. Metallicity also plays a role and leads to slightly larger 3D–1D differences at [M∕H] = 0.0. All these patterns are caused by a complex interplay between the radiation field, opacities, and horizontal temperature fluctuations that occur due to convective motions in stellar atmospheres. Although small, the 3D–1D differences in the magnitudes and colour indices are nevertheless comparable to or larger than typical photometric uncertainties and may therefore cause nonnegligible systematic differences in the estimated effective temperatures.
Key words: hydrodynamics / stars: atmospheres / techniques: photometric / techniques: spectroscopic
© ESO 2018
1 Introduction
Our understanding of stars relies on the analysis of their spectroscopic and photometric properties, which are studied with the aid of stellar model atmospheres. Obviously, physical realism of the model atmospheres is one of the key factors that define the reliability of the obtained results. Until now, 1D hydrostatic model atmospheres were the most widely used in studies of this kind. Amongst the advantages that make these models particularly attractive is that they combine sufficiently realistic physics with high computational speeds and the ease of use. Not surprisingly, a number of extensive 1D model atmosphere grids have been produced so far and have been widely used in many astrophysical contexts (e.g. ATLAS9, Castelli & Kurucz 2003; MARCS, Gustafsson et al. 2008; PHOENIX, Brott & Hauschildt 2005). Nevertheless, since these are 1D hydrostatic models, they cannot properly account for the multidimensional and timedependent nature of phenomena taking place in stellar atmospheres, such as convection, pulsations, shockwave activity.
A step beyond these limitations can be made by using stateoftheart 3D hydrodynamical model atmospheres. Currently, several 3D hydrodynamical model atmosphere codes are available for computing realistic model atmospheres of different types of stars, for example Bifrost (Gudiksen et al. 2011), CO^{5}BOLD (Freytag et al. 2012), MURaM (Vögler 2003; Vögler et al. 2005), and Stagger (Magic et al. 2013, and references therein). A quickly growing body of evidence shows that these models are indeed superior to their 1D counterparts in many aspects, including their ability to better reproduce observable properties of different types of stars: the Sun (Asplund et al. 2000; Caffau et al. 2008; Caffau et al. 2011; Steffen et al. 2015a), latetype dwarfs (González Hernández et al. 2009; Ramírez et al. 2009; Behara et al. 2010), subgiants (González Hernández et al. 2009; Amarsi et al. 2015), and red giants (Collet et al. 2007; Ramírez et al. 2010; Dobrovolskas et al. 2013). It is also important to note that the first grids of 3D hydrodynamical model atmospheres covering a range in T_{eff}, log g, and [M∕H] are already available for use (e.g. CIFIST grid produced using CO^{5}BOLD model atmospheres, Ludwig et al. 2009; the grid computed with the Stagger code, Magic et al. 2013). All these important developments form a solid basis for the wider use of 3D hydrodynamical models in stellar atmosphere studies.
Unfortunately, the influence of convection on the spectral energy distributions (SEDs), photometric magnitudes, and colour indices – and thus the potential advantages of using 3D model atmospheres in this domain – still remainslargely unexplored. In our earlier studies (Kučinskas et al. 2005, 2009), we used 3D hydrodynamical CO^{5} BOLD model atmospheresto compute photometric magnitudes and colour indices of a red giant located close to the red giant branch (RGB) tip (T_{eff} ≈ 3660 K, log g = 1.0, [M∕H] = 0.0). We found that convection plays a nonnegligible role in defining the SED, photometric magnitudes, and colour indices of this particular object, with noticeable 3D–1D differences in the colourindices (e.g. Δ(V − I) ≈ 0.14, Δ(V − K) ≈ 0.20) and, subsequently, differences in the effective temperature (determined using T_{eff} – colour calibrations) of up to ~60 K. A similar investigation was also performed by Casagrande (2009) for the Sun and a Ktype dwarf (T_{eff} = 4780 K, [M∕H] = 0.0). In this case, however, the 3D–1D differences in T_{eff} were smaller and did not exceed 10 K and 20 K, respectively. To our knowledge, these are the only studies where photometric magnitudes and colour indices of stars have been analysed using 3D hydrodynamical model atmospheres. As a consequence, the impact of convection on the spectrophotometric properties of stars in a wider atmospheric parameter space is still unknown.
We therefore performed a detailed investigation of the influence of convection on the SEDs, photometric magnitudes, and colour indices. The obtained results are summarized in a series of two papers. In the first paper, Bonifacio et al. (2018, hereafter Paper I), we presented grids of photometric colour indices and 3D–1D corrections in several widely used photometric systems, computed using 3D hydrodynamical CO^{5} BOLD and 1D hydrostatic LHD model atmospheres. These grids can be used to correct synthetic photometric colour indices for the 3D hydrodynamical effects and therefore can be applied to any type of study based on stellar photometry.
In the current study, which is the second paper in the series, we used a smaller set of 3D hydrodynamical CO^{5} BOLD and 1D hydrostatic LHD model atmospheres ranging from the MS to the RGB tip at two different metallicities, [M∕H] = 0.0 and − 2.0. Three types of model atmospheres were utilized to compute synthetic SEDs, photometric magnitudes, and colour indices: 3D hydrodynamical, averaged , and 1D hydrostatic (see Sect. 2.2 for details). We focused on a detailed comparison of the model predictions in order to understand the influence of convection on the spectrophotometric properties of stars across the H–R diagram.
The present paper is structured as follows. The methodology used to compute synthetic photometric magnitudes and colour indices is outlined in Sect. 2. The obtained results, including the computed SEDs of the Sun and Vega, and the SEDs and photometric magnitudes of the model atmospheres across the H–R diagram, as well as the influence of various model assumptions on the computed SEDs and magnitudes/colour indices, are presented and discussed in Sect. 3. Finally, the main results and conclusions are summarized in Sect. 4.
2 Methodology
2.1 General considerations
To assess the influence of convection on the spectrophotometric properties of various types of stars, we computed SEDs, synthetic magnitudes, and colour indices using a set of 3D hydrodynamical and averaged model atmospheres that were calculated with the CO^{5}BOLD code (Sect. 2.2.1). For comparison, we utilized 1D hydrostatic models computed with the LHD code (Sect. 2.2.2). Atmospheric parameters of the model atmospheres used were selected to span across those of stars located on the MS, main sequence turnoff (TO), subgiant branch (SGB), and RGB in various Galactic populations (Fig. 1). These model atmospheres were used to compute wavelengthdependent surface fluxes, F_{λ} (SEDs), for each given model atmosphere (Sect. 2.3). Finally, synthetic photometric magnitudes and colour indices were computed from the obtained SEDs in order to investigate the influence of convection on the spectrophotometric properties of these types of stars.
In this study we aimed at a strictly differential comparison of the observable properties predicted by the 3D hydrodynamical CO^{5} BOLD and 1D hydrostatic LHD model atmospheres. Hence, the 3D hydrodynamical, averaged , and 1D models used in our work were computed using identical atmospheric parameters (i.e. T_{eff}, log g, and [M∕H]), chemical composition, opacities, and equation of state. To obtain SEDs that were subsequently used for the computation of photometric magnitudes and colour indices, we used the code NLTE3D intended to solve the restricted nonlocal thermodynamic equilibrium (NLTE) problem in three spatial dimensions. Rather conveniently for our purposes, the code computes wavelengthdependent mean intensities and surface fluxes, F_{λ} (in LTE, Sect. 2.3), which can be used to calculate photometric magnitudes and colour indices. We therefore tried to homogenize the input physics and numerical details of the model and spectral synthesis computations as much as possible so that the differences between the photometric magnitudes and colour indices could be traced back to the sole influence of convection. It is for these reasons that we refrained from referencing one of the widely used 1D hydrostatic model atmospheres as 1D comparison models (e.g. ATLAS9), because this choice would have led to additional differences in the assumptions and input physics between the 3D and 1D models, and thus to additional systematic differences in the computed fluxes and photometric magnitudes and/or colour indices.
Despite this, one important remaining inconsistency is that both in the present paper and the companion Paper I, opacities used in the computation of the model atmospheres and SEDs were slightly different (see Sect. 2.3 for details). In addition, CO^{5} BOLD and LHD model atmospheres, as well as their SEDs, were computed treating scattering as true absorption. Nevertheless, since we were interested in a differential 3D–1D comparison of the magnitudes and colour indices, the impact of these inconsistencies on the results is minor (see Sect. 2.3 and Paper I for further details and discussion).
Fig. 1 3D hydrodynamical CO^{5}BOLD and 1D hydrostatic LHD model atmospheres used in this work, shown in the log g–T_{eff} plane (large yellowfilled circles). Different isochrones (Pietrinferni et al. 2004, 2006) indicate the approximate loci of stars in the Galactic thin and thick disk, bulge, and halo. 

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2.2 Model atmospheres
2.2.1 Threedimensional hydrodynamical and averaged CO^{5} BOLD model atmospheres
All 3D hydrodynamical stellar model atmospheres used in our study were computed as part of the CIFIST model atmosphere grid (Ludwig et al. 2009). Simulations were performed using the CO^{5} BOLD code which solvestimedependent radiationhydrodynamics equations in Cartesian geometry (see Freytag et al. 2012, for details). All model runs were long enough to cover between five and ten convective turnover timescales, as measuredby the Brunt–Vaisälä timescale. Solarscaled abundances from Grevesse & Sauval (1998) were used in the simulations, except that for CNO the values recommended by Asplund et al. (2005) were adopted: A(C)= 8.41, A(N)= 7.80, and A(O)= 8.67. Models at [M∕H] = −2.0 were computed with a constant alphaelement enhancement of . Monochromatic MARCS opacities (Gustafsson et al. 2008) were divided into five and six opacity bins for the models at [M∕H] = 0.0 and − 2.0, respectively. The scattering was treated as true absorption. All model simulations were done in LTE (see Ludwig et al. 2009, for more details on the model calculations). A list of the 3D hydrodynamical models used in this work and their parameters are provided in Table 1.
To speed up the computation of wavelengthdependent surface fluxes, for each 3D hydrodynamical model from Table 1 we selected a sample of 20 equidistantly spaced 3D model structures that were computed at different instants in time (snapshots). The snapshots were selected from the entire model simulation run such that the most important statistical properties of the entire model sequence would be also preserved in the 20 snapshot subsample^{1}. Since each snapshot is characterized by slightly different total surface flux, and thus effective temperature, in Table 1 we also provide RMS variation in T_{eff} in each given snapshot ensemble.
We also used averaged model atmospheres which were computed by averaging individual 3D model structures in each of the 20 snapshot subsamples on surfaces of equal Rosseland optical depth. In fact, the averaged structures are 1D model atmospheres, thus they no longer carry the imprints of the horizontal fluctuations of hydrodynamical and thermodynamic quantities. Therefore, analysis of the 3D– differences helps us to assess the importance of horizontal fluctuations on the emergent surface fluxes, photometric magnitudes, and colour indices (see Sect. 3.3).
2.2.2 Onedimensional LHD model atmospheres
Onedimensional hydrostatic model atmospheres were computed with the LHD model atmosphere code (Caffau et al. 2008) in which convection was treated using the mixinglength theory in the formulation of Mihalas (1978). Stellar parameters, opacities, equation of state, and chemical composition used to compute the LHD models were identical to those used in the CO^{5} BOLD simulations. In the standard setup, the mixinglength parameter was set to α_{MLT} = 1.0. However, totest the sensitivity of the SEDs, photometric magnitudes, and colour indices on the choice of α_{MLT}, additional LHD models were computed with α_{MLT} = 0.5 and 2.0 (seeSect. 3.3.3). We note, however, that the mixing length parameter was utilized only with the 1D LHD hydrostatic models; in the 3D hydrodynamical (and averaged ) models the convective flux was modelled using the timedependent equations of radiation hydrodynamics. A list of 1D LHD modelatmospheres and their parameters is given in Table 2.
2.2.3 Model atmospheres of the Sun and Vega
In order to validate the accuracy and realism of our model atmospheres, we compared synthetic solar SEDs computed using 3D hydrodynamical, averaged , and 1D hydrostatic model atmospheres with the observed solar flux spectrum. For this, we used the CO^{5} BOLD and LHD models of the Sun from Steffen et al. (2015a). These are currently the most advanced solar models computed using the CO^{5} BOLD and LHD codes (see Steffen et al. 2015a, for details). Therefore, by utilizing them we tried to ensure that the best theoretical models were used to compare their predictions with the observations.
Similar comparison was also made in the case of Vega. Since its atmosphere is fully radiative, it was neither possible nor desirable to compute a 3D hydrodynamical model of Vega because the flux of such a model should be identical to that of the 1D LHD model atmosphere. Thus, to compare the observed and theoretical SEDs, we used the 1D LHD and ATLAS9 models of Vega (the former model was also used to compute the magnitude zero points for Vega, see Sect. 2.3). The atmospheric parameters of Vega adopted for the 1D LHD model atmosphere calculations were T_{eff} = 9550 K, log g = 3.95, and [M∕H] = −0.5, with an enhancement in αelement abundances of . Just as for the cooler CO^{5}BOLD and LHD models in our sudy, the elemental abundances used in the computation of the Vega 1D LHD model were taken from Grevesse & Sauval (1998), with the updates on CNO abundances from Asplund et al. (2005). The equation of state used to produce a 1D LHD model of Vega was identical to that utilized in the computation of all other CO^{5}BOLD and LHD models listed in Tables 1 and 2. We used a 12bin opacity table based on Hayek’s approximation in which scattering was treated as true absorption in the deeper layers and was ignored in the outer ones (see Paper I for further discussion on scatteringrelated issues). The ATLAS9 SED of Vega was taken from Castelli & Kurucz (1994).
Threedimensional hydrodynamical CO^{5}BOLD model atmospheres.
Onedimensional hydrostatic LHD model atmospheres.
2.3 Spectral energy distributions, photometric magnitudes, and colour indices
The wavelengthdependent surface fluxes, F_{λ}, of the 3D hydrodynamical, averaged , and 1D hydrostatic model atmospheres were computed using NLTE3D package. This package is designed to compute NLTE departure coefficients, b_{i} (x, y, z), at each geometrical position (x, y, z) in the 3D model atmosphere box and for each energy level i of a given model atom (for details regarding the NLTE3D code see Steffen et al. 2015a). The NLTE3D code also computes wavelengthdependent mean intensity at each geometrical position in the model atmosphere, J_{λ} (x, y, z), as well as the emergent flux at the top of the atmosphere, F_{λ}, which can be used to calculate photometric magnitudes and colour indices. Continuum opacities used in the NLTE3D code were computed with the IONDIS and OPALAM routines, which are also employed in the Linfor3D spectral synthesis code (Steffen et al. 2015b). These are different from the MARCS continuum opacities that were used to produce the binned opacity tables employed in the CO^{5}BOLD and LHD simulations. Line opacities used in the computation of SEDs were taken into account by utilizing LITTLE opacity distribution functions (ODFs) from the ATLAS9 model atmosphere package (Castelli & Kurucz 2003). Both choices lead to inconsistencies between the opacities used in the calculations of SEDs (and thus photometric magnitudes and colour indices) and those employed in the computation of the CO^{5}BOLD and LHD models.
As a consequence, wavelengthintegrated surface fluxes obtained from the SEDs that were computed using different model atmospheres were slightly inconsistent, even though the effective temperatures of all models were identical. To correct for this mismatch, we renormalized the SEDs of the 3D, , and 1D models to their nominal effective temperatures using wavelengthindependent scaling factors. This was not done in Bonifacio et al. (2017) and Paper I. The differences in the 3D–1D corrections due to the different approaches used in the two studies were in fact very small and did not exceed 0.001 mag.
For the calculation of magnitudes and colour indices we used standard ATLAS9 LITTLE ODFs computed with the microturbulence velocity set to ξ_{mic} = 2 km s^{−1}. However, in order to assess a possible influence of this choice on the 3D–1D corrections for magnitudes and colour indices, we also used ODFs computed with ξ_{mic} = 1.0 km s^{−1} (Sect. 3.3.3). The wavelengthdependent surface fluxes, F_{λ} (SEDs), were calculated at 1048 wavelength points spread nonequidistantly between 133.5 and 99 799 nm. The blue wavelength limit was chosen to allow for the computation of nearUV photometric magnitudes and colour indices (see Paper I).
From the obtained SEDs we computed photometric magnitudes and colour indices in the JohnsonCousins UBVRI, 2MASS JHK_{s}, and Strömgren uvby photometric systems. The UBVRIJHK_{s} system was chosen because it is well defined and its bandpasses are located in the wavelength range that extends over those of other widely used broadband photometric systems, such as SDSS ugriz. Therefore, by estimating the influence of convection on the UBVRIJHK_{s} magnitudes and colour indices one can obtain a rough idea regarding the size of 3D–1D corrections expected at similar wavelengths for other broadband photometric systems. The mediumband Strömgren uvby photometric system was chosen because its bandpasses are mostly located in the blue part of the spectrum where, as we will see in Sect. 3.3.1, the influence of 3D effects is greatest. On the other hand, its filter transmission curves are relatively narrow. At certain wavelengths where the 3D–1D differences are largest, the Strömgren’s magnitudes and colour indices may be affected more strongly than those in the UBVRIJHK_{s} system, thereby allowing us to assess the influence of convection on magnitudes and colour indices in the photometric bands of different width.
Synthetic magnitudes computed in both photometric systems were normalized with respect to Vega. For this, we followed Bessell & Murphy (2012) and assumed the UBVRI magnitudes of Vega equal to 0.03, while for the 2MASS bands we used J = 0.001, H = −0.005, and K_{s} = 0.001, in order to be consistent with the zeromagnitude fluxes provided by Cohen et al. (2003). For the Strömgren bands, we utilized Vega magnitudes from Maíz Apellániz (2007). The filter transmission curves for the computation of the zero points and photometric magnitudes were taken from Bessell & Murphy (2012) for the JohnsonCousins UBVRI bands and from Cohen et al. (2003) for the 2MASS JHK_{s} bands. For the Strömgren uvby system, we used the filter transmission curves from Maíz Apellániz (2006).
At variance with Bonifacio et al. (2017) and Paper I, where we assumed an angular diameter for each model atmosphere and applied to the synthetic flux the same zero points that were applied to colour indices, in this paper we have chosen to determine the zero points of the synthetic colour indices using our 1D LHD model atmosphere of Vega. The magnitude zero points in the different filter bands were obtained using the SED computed with the 1D LHD model atmosphere of Vega and applied to synthetic magnitudes calculated with the 3D hydrodynamical, averaged , and 1D hydrostatic models. The obtained magnitude zero points were in good agreement with those determined in other studies; for example, the differences between our zero points and those determined by Casagrande & VandenBerg (2014) did not exceed 0.01 mag.
We note, however, that in both papers we were interested in a strictly differential comparison of fluxes, photometric magnitudes, and/or colour indices, i.e., the differences between these quantities computed using 3D and 1D model atmospheres. In this situation, the choice of particular zero points is irrelevant because in the differential comparison of 3D–1D magnitude differences they cancel out. Considering the limitations in the model physics due to our treatment of scattering (see Paper I for details), we discourage the use of our colour indices or magnitudes and recommend using only the 3D–1D colour corrections.
3 Results and discussion
3.1 Spectral energy distribution of the Sun
A comparison between the synthetic solar SEDs computed using 3D hydrodynamical CO^{5}BOLD and 1D hydrostatic LHD model atmospheres with the observed solar absolute calibrated flux spectrum of Neckel & Labs (1984) and taken from the ftp site as provided in Neckel (1999) is shown in Fig. 2. The observed spectrum was resampled to the resolution of the synthetic SEDs, while the latter were scaled to the distance of one astronomical unit and one solar radius. In the case of the 3D hydrodynamical and averaged models, the SEDs were computed using the 20snapshot ensemble, as described in Sect. 2.2.1 (see also Steffen et al. 2015a). We emphasize that this is a comparison on an absolute scale, i.e., no fitting was performed.
As seen in Fig. 2, the differences between SEDs computed using 3D hydrodynamical and 1D hydrostatic model atmospheres are generally very small and never exceed a few percent. Nevertheless, certain systematic differences are apparent as well. For example, a 3D hydrodynamical model produces more flux in the blue and less flux in the red part of the spectrum (we note that the synthetic SED of the 1D model was normalized to produce the same wavelengthintegrated flux as that of the 3D hydrodynamical model). The observed SED was not corrected for telluric absorption, thus larger deviations between the observed and synthetic SEDs are apparent in the red and infrared parts of the spectrum. Towards the blue, a slight tendency towards excessive flux in the synthetic SEDs is apparent, with the exception of a region around the Hγ line. Nevertheless, the correspondence between calculated and observed solar SEDs is in general very satisfactory, in particular considering the rather sensitive ultraviolet wavelength region.
Fig. 2 Comparison of theoretical and observed SEDs of the Sun. Top: solar SEDs computed using 3D hydrodynamical CO^{5} BOLD (green solid line) and 1D LHD (red dotted line) model atmospheres, plotted together with the observed absolute solar flux spectrum from Neckel (1999, black solid line). Bottom: relative differences between the SEDs: observed–3D (black solid line) and 3D–1D (red dashed line, scale on the right yaxis). 

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3.2 Spectral energy distribution of Vega
A comparison of the observed and synthetic SEDs of Vega is shown in Fig. 3. For this, we used 1D hydrostatic model atmospheres computed with the ATLAS9 and LHD codes. Because of inconsistencies in the opacities used to compute the 1D LHD model of Vega and its SED (Sect. 2.3), the LHD SED of Vega was renormalized to produce the same flux as that of the ATLAS9 model. The observed SED of Vega was taken from the HST CALSPEC library^{2} and was resampled to the spectral resolution of synthetic SEDs. For the comparison, synthetic SEDs were scaled to the distance of Vega (7.69 pc, van Leeuven 2007) and the radius of Vega (2.818 R_{⊙}, Yoon et al. 2010). The scaled SEDs were then directly compared with the HST CALSPEC SED of Vega, i.e., no fitting was done.
As in the case of the Sun, the agreement between the observed and synthetic SEDs is very good in the entire wavelength range covered in Fig. 3. Larger differences are seen in the regions around strong lines (mostly those of hydrogen), which in extreme cases may reach 10%. Some systematics are seen, too: the flux in the HST CALSPEC SED is slightly lower in the UV and somewhat higher in the IR parts of the spectrum. Nevertheless, the typical differences are small and do not exceed ± 2 %. The fluxes of the two 1D hydrostatic models, ATLAS9 and LHD, are also very similar although there are small differences, on the level of a few percent, in the UV and optical parts of the spectrum.
As a final remark, it is worth mentioning that Vega is too complex an object to model with the standard model atmospheres. For example, the abovementioned IR excess of the observed spectrum over that of the LHD model is expected because Vega is known to possess a circumstellar disk (see discussion in Bohlin 2014). In addition, Vega is a rapid rotator and this may also have an impact on the structure of its atmosphere and, thus, on the observable properties. Finally, because of its rapid rotation there may be other effects, for example, those related to gravity darkening that are not yet taken into account in the current model atmospheresof Vega. Therefore, certain systematic differences between the observed HST CALSPEC spectrum and the synthetic LHD and ATLAS9 SEDs of Vega are to be expected. What our comparison shows is that these differences are nevertheless relatively small.
Fig. 3 Comparison of theoretical and observed SEDs of Vega. Top: SEDs of Vega computed using 1D hydrostatic LHD (red dotted line)and ATLAS9 (blue dashed line) model atmospheres, plotted together with the HST CALSPEC absolute calibrated flux spectrum of Vega from the HST CALSPEC library (black solid line). The close overlap of the three lines makes it difficult to distinguish between them. Bottom: relative differences between the SEDs: HST CALSPEC – LHD (red dotted line) and HST CALSPEC – ATLAS9 (blue dashed line). 

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3.3 Spectral energy distributions and photometric properties of MS, TO, SGB, and RGB stars
3.3.1 Spectral energy distributions
Spectral energy distributions computed with the 3D hydrodynamical model atmospheres, as well as differences between the SEDs obtained using 3D hydrodynanical and 1D hydrostatic models, are shown in Fig. 4. A common tendency is that 3D hydrodynamical models tend to predict more flux in the UV and less in the IR part of the spectrum. In the UV, the 3D–1D differences quickly diminish with increasing effective temperature, i.e., they are largest in cool MS and RGB stars, and smallest in TO stars. The influence of gravity, on the other hand, is small.
Following our considerations presented in Appendix A, higher flux in the UV and lower in the IR should be expected in the presence of horizontal temperature fluctuations alone, i.e., even if their effect on the opacities is not taken into account. This is confirmed by a comparison of realistic SEDs computed using the 3D, averaged , and 1D model atmospheres of RGB and TO stars (Fig. 5). In the coolest red giants, higher flux in the UV is mostly caused by horizontal temperature fluctuations in the 3D hydrodynamical model atmosphere, as traced by the 3D– differences in Fig. 5 (top row). In the IR, the horizontal fluctuations and differences between the average temperature profiles in the and 1D model atmospheres play a comparable role, with the joint effect typically leading to lower flux in the IR (λ ≥ 1000 nm). Similar behaviour is seen in the SEDs of MS stars too, although the total effect, especially in the UV, is smaller (Fig. 5, bottom row). In part, this is caused by the negative –1D differences, especially in the lowmetallicity model. Our tests have shown that continuum flux in the UV typically forms in the deeper atmospheric layers where horizontal temperature fluctuations are larger, while the formation of IR continuum is confined to the outer layers where fluctuations are smaller. In addition, differences between temperature profiles of the averaged and 1D models are also larger in the deeper atmosphere. All together, this leads to a larger cumulative effect in the UV than in the IR and, consequently, to larger 3D–1D differences in the UV.
As far as the role of opacities is concerned, the largest contribution comes from the boundbound transitions, which in the computation of SEDs were taken into account using ATLAS9 ODFs. This is illustrated in Fig. 6, which displays differences between the SEDs computed using 3D, , and 1D models, with the ODFs switched on and off. The results of this test show that line opacities (often referred to as “line blanketing”) indeed have a huge influence on the resulting SEDs of solar metallicity models. Their contribution gradually becomes dominant towards the shorter wavelengths (λ ≤ 600 nm) where spectral lines of various metals become more abundant. As expected, at [M∕H] = −2.0 the effect of lineopacity is smaller although still nonnegligible. We recall, however, that this is the situation when scattering is treated as true absorption; the overall picture may be different when scattering is properly taken into account.
Fig. 4 Top: SEDs corresponding to the 3D hydrodynamical CO^{5}BOLD models listed in Table 1. Bottom: relative flux difference between the SEDs computed using 3D hydrodynamical CO^{5} BOLD and 1D hydrostatic LHD model atmospheres. Left panels: [M∕H] = 0.0; right panels: [M∕H] = −2.0. 

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Fig. 5 SEDsof the RGB (top row) and TO (bottom row) models computed using 3D hydrodynamical, averaged, and 1D hydrostatic model atmospheres, at [M∕H] = 0.0 (left) and [M∕H] = −2.0 (right). Top panels: SEDs corresponding to different models. Bottom panels: relative differences between the SEDs shown in the corresponding top panels. All SEDs were renormalized to yield the same effective temperature. 

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Fig. 6 Relative differences between the SEDs of RGB (top row) and TO (bottom row) stars computed with and without ODFs using 3D hydrodynamical, averaged , and 1D hydrostatic model atmospheres, at [M∕H] = 0.0 (left) and [M∕H] = −2.0 (right). 

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3.3.2 Photometric magnitudes and colour indices
A glance at the differences between UBVRIJHK_{s} magnitudes computed using the 3D and 1D model atmospheres (Fig. 7) reveals similar patterns to those seen in the comparison of the SEDs (Sect. 3.3.1). In particular, (a) 3D models tend to produce more flux in the UV and less in the IR; (b) differences in the magnitudes and colour indices, especially those with filter bands located in the blueUV part of the spectrum, become smaller with increasing effective temperature of the model atmosphere; (c) at the highest effective temperatures, the differences are somewhat more pronounced in the lowmetallicity models. Interestingly, in the metalpoor models the initially positive 3D–1D differences in the bluest bands quickly decrease in their absolute size with increasing effective temperature and gradually become negative for models characterized with the highest effective temperatures. A similar pattern is seen in the case of magnitudes and colour indices in the Strømgren system (Fig. 8). Overall, the 3D–1D differences in the two photometric systems are small and generally are well within ± 0.1 mag, for magnitudes and for colour indices. As discussed in Sect. 3.3.1, the 3D–1D differences in the magnitudes and colour indices are mostly caused by horizontal temperature fluctuations in the 3D hydrodynamical model atmospheres which affect both the source function and opacities.
3.3.3 The impact of various modelling assumptions on synthetic colours
The mixing length parameter
It is known that the choice of the mixing length parameter, α_{MLT}, which controls the efficiency of convective mixing and has a direct influence on the thermal structure of the 1D hydrostatic model atmosphere, may affect the observable properties of a given model atmosphere. In the context of our study, α_{MLT} was used in the computations of 1D LHD model atmospheres which were utilized in the differential 3D–1D analysis of photometric magnitudes and colour indices. Our standard LHD models were computed with α_{MLT} = 1.0. To investigate the influence of this choice on the spectrophotometric properties of the LHD models, we computed a set of additional LHD models with α_{MLT} = 0.5 and 2.0. In Figs. 9 and 10 we show differences in the photometric magnitudes and colour indices of the LHD models computed with α_{MLT} = 0.5 and 2.0 and those computed with α_{MLT} = 1.0. The resulting differences in the 3D–1D corrections will be of the same size.
As expected, in the metalpoor models different choices of α_{MLT} lead to larger differences in the photometric magnitudes and colour indices because in this case the convective envelope penetrates closer to the optical surface than it does in the solar metallicity models (see e.g. Kučinskas et al. 2013a). Despite this, the differences are small, and for both magnitudes and colour indices are confined to ≈ ± 0.025 mag.
Fig. 7 3D–1D magnitude differences in the UBVRIJHK_{s} photometric system computed using 3D hydrodynamical CO^{5}BOLD and 1D hydrostatic LHD models, at [M∕H] = 0.0 and −2.0. 

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Fig. 8 Same as Fig. 7, but in the Strømgren photometric system. 

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Fig. 9 Differences in the UBVRIJHK_{s} magnitudes obtained from the 1D LHD models that were computed using different mixing length parameters, plotted as differences with respect to the models computed with α_{MLT} = 1.0. Dotted horizontal lines mark zero magnitude differences. The yscale increases downwards and the zero difference lines are shifted incrementally by +0.05 mag from top to bottom. 

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Fig. 10 Same as Fig. 9, but for the colour indices. 

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The role of scattering
The CO^{5}BOLD and LHD model atmospheres used in our study were computed by treating scattering as true absorption (Ludwig et al. 2009; Freytag et al. 2012). The identical procedure was applied when computing SEDs with the NLTE3D code from the 3D, averaged , and 1D models. The main reasons behind this choice was that it reduces the complexity of radiative transfer (RT) calculations and increases the computational speed dramatically^{3}. Several recent studies have focused on the validity of this approach in the context of 3D hydrodynamical modelling of stellar atmospheres with different model atmosphere codes (Hayek et al. 2010; Collet et al. 2011; Ludwig & Steffen 2012). While the obtained results are somewhat inconclusive regarding how much the thermal structure of the atmosphere may be affected by this choice, it is clear that scattering makes an important contribution to the emergent radiation field in the blueUV part of the spectrum, especially in the metalpoor regime.
In our companion paper we therefore investigated a possible impact of this simplified approach on the spectrophotometric properties of the model atmospheres computed with the CO^{5}BOLD code (Paper I). For this, we used two CO^{5}BOLD models computed with identical atmospheric parameters but different treatment of scattering, (a) with scattering treated as true absorption, and (b) with scattering treated in the Hayek approximation, which is deemed to be a sufficiently accurate substitute for a more complex approach where scattering is treated fully consistently. These models were used to compute photometric colour indices, again with (a) scattering treated as true absorption, and (b) by performing fully consistent computations of scattering. We refer the reader to Paper I for the indepth discussion of the results obtained in this test, and here we only briefly note that scattering was indeed found to be important in the blueUV part of the spectrum. Fortunately, the 3D–1D differences in the colour indices computed using different approaches in the treatment of scattering were always consistent to within 0.03 mag, even when the bluest colour indices were involved (see Sect. 2.3 in Paper I).
Radiative transfer computations
To speed up the RT computations, the radiative field in the 3D hydrodynamical models is frequently computed on a coarser grid than that used in the model simulations, for example, at each third horizontal point of the original grid (e.g. Kučinskas et al. 2013b; Dobrovolskas et al. 2013). This effectively reduces the number of grid points where the radiation field is computed significantly, which speeds up the computations. Normally, this procedure does not introduce significant differences even in the computation of spectral line profiles, which are typically rather sensitive to the properties of the grid resolution (Kučinskas et al. 2013b).
In the present study we did not use this simplification. Instead, the emergent flux was computed at each grid point of the model atmosphere.Nevertheless, we performed RT calculations with a coarser grid using only each third horizontal point of the original grid to estimate the possible effect of this frequently used choice on the emergent flux. For this test, we used a single snapshot of the CO^{5}BOLD model of a red giant star with T_{eff} = 4000 K, log g = 1.5, and [M∕H] = 0.0. This choice was motivated by the fact that in these cool and lowgravity red giants horizontal temperature fluctuations are characterized by very steep gradients and large amplitudes, which makes these stars good targets for such a test.
The SEDs computed using the original and coarser numerical grids are shown in Fig. 11. The differences typically do not exceed 0.5% in the opticalIR range but they increase rapidly with decreasing wavelength at ~300 nm and may grow alarmingly large below ~250 nm. This, however, has a negligible effect on the magnitudes and colour indices in the UBVRIJHK_{s} and Strømgren systems as their filter transmission curves are located at wavelengths longer than 300 nm.
Fig. 11 Top: SEDs computed using the original grid of the model atmosphere (kskip = 1) and a coarser grid covering each third cell of the original grid (kskip = 3). A single snapshot of the 3D hydrodynamical model of a red giant was used in the computation of both SEDs. Bottom: differences between the two SEDs shown in the top panel. 

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Effects related to opacities
Two aspects should be mentioned here. First, as was already discussed in Sect. 2.3, opacities used in the computation of the model atmospheres and those utilized in the calculation of SEDs were slightly inconsistent: the CO^{5}BOLD and LHD models were computed using binned MARCS opacities, while the SEDs and magnitudes and colour indices were computed using monochromatic continuum opacities from the Linfor3D code together with the line opacities using ODFs from the ATLAS9 package. Fortunately, in the context of differential comparison of the 3D and 1D model predictions these inconsistencies should not pose a serious problem since their effects will be expected to largely cancel out.
Second, we used binned opacities in the computation of CO^{5}BOLD and LHD modelatmospheres. The main advantage of using opacity binning scheme, which is described in detail in Nordlund (1982), Ludwig et al. (1994), and Vögler et al. (2004), is that the model computations are significantly faster. This occurs because using even a relatively small number of opacity bins it is possible to maintain a sufficiently realistic heating/cooling balance in the model atmosphere. A question is, of course, how many bins should be deemed sufficient as this will obviously depend on the task at hand. We recall that the standard CO^{5}BOLD and LHD models utilized in the present study were computed using five and six opacity bins at [M∕H] = 0.0 and − 2.0, respectively. To test whether this number of bins indeed provides the required accuracy in the model computations, we also computed a test CO^{5}BOLD and LHD models with T_{eff} = 5000 K, log g = 2.5, and [M∕H] = −2.0 and the opacities grouped into 14 bins. Indeed, the differences in the magnitudes produced using the two models are minor (Fig. 12), thus confirming the validity of the coarser binning scheme for the computation of SEDs, as well as the photometricmagnitudes and colour indices.
Fig. 12 Effects of opacity binning on the photometric magnitudes in the UBVRIJHK_{s} system. The plot shows differences in the magnitudes of two 3D hydrodynamical CO^{5} BOLD models computed using opacities grouped into 14 and 6 opacity bins. 

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Effects of the microturbulence velocity
The standard ODFs from the ATLAS9 package that were used to account for the line opacities in the computations of SEDs with the NLTE3D code were computed using the microturbulence velocity ξ_{mic} = 2.0 km s^{−1} (Castelli & Kurucz 1994). In order to test how sensitive the computed SEDs and photometric magnitudes and colour indices were to this choice, we produced an additional set of SEDs using ATLAS9 ODFs computed with ξ_{mic} = 1.0 km s^{−1}. The obtained SEDs of the 3D, , and 1D model atmospheres are shown in Fig. 13. The differences between SEDs computed using the two values of microturbulence velocity are almost always below ≈1%, except in the blue part of the spectrum (λ < 400 nm) where in extreme cases they may reach ≈4% at 300 nm.
Fig. 13 Effects of microturbulence velocity used calculating opacity distribution functions on the spectral energy distribution. The plot shows relative 3D–1D, 3D–<3D>, and <3D>–1D differences in the flux (normalised to that of the corresponding 3D model) of several model atmospheres computed using opacities with microturbulence velocities of 2.0 and 1.0 km s^{−1}. 

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Open issues and future work
Results obtained in our study show that SEDs – and thus photometric magnitudes and colour indices – are most sensitive to the influence of convection in the blueUV part of the spectrum. The 3D–1D differences are largest there and tend to increase with decreasing wavelength. It is important to stress that at these wavelengths the influence of the chromospheric layers becomes increasingly important too. For example, using our first exploratory 3D hydrodynamical CO^{5}BOLD model of a cool red giant in which the outer atmospheric layers were extended to mimic a chromosphere (T_{eff} = 4000 K, log g = 1.5, and [M∕H] = 0.0), we found that the influence of chromosphere on the emergent model flux becomes significant bluewards of ~300 nm (Wedemeyer et al. 2017). This is caused by additional heating in the outer chromosphere which leads to higher flux in the blueUV. In fact, this influence is already noticeable at 1000 nm, but the differences start to exceed the level of 10% only at ≤350 nm. Obviously, our exploratory model was still too simplistic to properly account for the physical complexity of real stellar chromospheres. Nevertheless, this test clearly demonstrated that extending the realism of the current 3D hydrodynamical model atmospheres in this domain may be crucial for reliable emergent flux computations in the blueUV part of the spectrum.
It also unclear whether the numerical resolution of the model grid used in the 3D hydrodynamical simulations may also have an influence on the emergent SEDs, just as it does on the properties of spectral lines.
Finally, NLTE effects may also play a role, especially in the formation of emergent flux in the blueUV part of the spectrum. Until now, however, NLTE effects could only be taken into account when modelling the formation of spectral lines of selected chemical elements with 3D hydrodynamical models. Therefore, the broader impact of these effects on the formation of continuum flux and line spectrum over a wider wavelength range is still unknown. Studies made using 1D hydrostatic model atmosphereshave shown that there is a noticeable influence on the resulting SEDs if the line blanketing in the model atmospheresis computed in NLTE, in particular with the lower flux predicted in the UV part of the spectrum (see e.g. Short et al. 2012, and references therein). Due to large horizontal inhomogeneities in the 3D hydrodynamical models and additional heating in the lower chromosphere, the impact of NLTE effects may be expected to become even more significant, especially in the UV, and thus will not completely cancel out when computing the 3D–1D corrections.
The bottom line therefore is that although the 3D–1D differences are largest in the blueUV part of the spectrum, the SEDs in this wavelength range are also very sensitive to a variety of other effects, as discussed above. Therefore, one should be generally cautious with the predictions made using current generations of the model atmospheres in this wavelength range.
4 Summary and conclusions
We studied the influence of convection on the SEDs and photometric colour indices of stars accross the H–R diagram. For this, we used 3D hydrodynamical CO^{5}BOLD and 1D hydrostatic LHD model atmospheres and computed their emergent wavelengthdependent fluxes (SEDs), which were further used to calculate magnitudes and colour indices in the JohnsonCousins UBVRI, 2MASS JHK_{s}, and Strømgren uvby photometric systems. To assess the effect of the 3D–1D differences in the magnitudes and colour indices on stellar population studies, the model atmospheres were selected in such a way that their atmospheric parameters would cover a range occupied by stars in different Galactic populations, such as Galactic disk, bulge, and halo.
The obtained results (Figs. 7 and 8) show that the 3D–1D differences in the magnitudes and colour indices are generally small in both UBVRIJHK_{s} and uvby photometric systems. Typically, the influence of convection is largest in the blueUV part of the spectrum and is most strongly pronounced at lowest effective temperatures. The strongest effect is seen in cool red giants where the 3D–1D differences in the JohnsonCousins U and Strømgren u bands may reach ≈ −0.2 mag at [M∕H] = 0.0 and to ≈ −0.1 mag at [M∕H] = −2.0. Noticeable differences are also seen in these bands in the MS and TO stars at [M∕H] = −2.0, although in this case they are of opposite sign and smaller, ≈ +0.05 mag. Nevertheless, in the majority of photometric bands the effect is significantly smaller and the 3D–1D differences typically do not exceed ± 0.03 mag. The effect of metallicity is strongest in the blue bands, but even in extreme cases the differences do not exceed ≈0.1 mag for magnitudes and colour indices computed at [M∕H] = 0.0 and − 2.0. The influence of gravity is generally negligible in all bands studied.
While small, the 3D–1D differences in magnitudes and colour indices cannot be deemed unimportant. For example, even a relatively minor 3D–1D difference of Δ(V − I) = 0.03 in cool red giants is comparable to or larger than the typical uncertainty of photometric measurements and may lead to a difference in the effective temperatureof ≈ 60 K. Moreover, the size of 3D–1D effects depends on the effective temperature, which will translate into different temperature corrections for cooler and hotter stars.
Finally, we would like to stress that current 3D hydrodynamical models are obviously not free from different shortcomings and limitations. For example, scattering was treated as true absorption when computing the grid of 3D hydrodynamical CO^{5}BOLD model atmospheresthat were used in this study. This may have an effect on the photometric magnitudes and colour indices, especially those located in the blueUV part of the spectrum where the sensitivity to the effects of convection is most pronounced. Although our tests have shown that the impact of this and other modelling assumptions on the resulting 3D–1D differences in the photometricmagnitudes and colour indices typically does not exceed a few hundredths of a magnitude, further improvements should certainly be expected with the arrival of next generation grids of 3D hydrodynamical model atmospheres.
Acknowledgements
We thank G. Ambrazevičiūtė, V. Dobrovolskas, and D. Prakapavičius for their input during the various stages of this project. We also thank V. Vansevičius for the useful comments and discussions. This research was funded by a grant (MIP089/2015) from the Research Council of Lithuania. HGL and AK acknowledge financial support by the Sonderforschungsbereich SFB 881 “The Milky Way System” (subproject A4) of the German Research Foundation (DFG). HGL and MS acknowledge funding from the Research Council of Lithuania for the research visits to Vilnius.
Appendix A A simplemodel of the colour corrections
To aid the interpretation of the calculated 3D–1D corrections of photometric magnitudes and colour indices, we developed a simple model that qualitatively captures their behaviour. To this end, we envision the star as radiating like a black body. In the 3D case temperature fluctuations are present so that the radiative output stems from an ensemble of radiators of different temperature. The 1D case is described by a single temperature T. The temperature fluctuations are characterized by their dispersion σT. Since it is a rough model we derive the formulae to leading order in σT ∕T only. As a normalization condition for the ensemble of blackbody radiators we obtain (A.1)
where σ is the Stefan–Boltzmann constant and B_{λ} the Planck function given by (A.2)
where c is the speed of light, k is the Boltzmann constant, and h is the Planck constant. The argument of B_{λ}(λ, T + σT) in Eq. (A.1) is intended to indicate the expectation value of the intensity emitted by the ensemble of blackbody radiators. Expanding to the second order in ΔT (the linear order vanishes) we obtain (A.3)
where the primes indicate derivatives with respect to T. Evaluating the second derivative yields (A.4)
Figure A.1 depicts flux ratios as given by formula (A.3) for various values of the mean temperature T assuming a fixed temperature dispersion of σT∕_{T} = 4%. The dispersion corresponds to an intensity contrast of roughly 16% which is typical for the latetype stellar atmospheres studied here. From the figure some qualitative aspects of the colour corrections can be expected: i) the corrections become larger towards the blue part of the spectrum; ii) the corrections are greater for stars of low effective temperature; iii) the corrections have different signs in the blue and red. We emphasize that the model is only rough, and leaves out the important response of the opacity to temperature fluctuations. Nevertheless, the detailed calculations show similarities to the predictions from the simple model.
Fig. A.1 Flux ratios as predicted the simple model given by Eq. (A.3). For the plot we assumed a temperature fluctuation of σ_{T}∕T = 4%. 

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The average effective temperature, T_{eff}, and its standard deviation, mean velocity at optical depth unity, mean velocity profile, and residual mass flux profile (see e.g., Caffau & Ludwig 2007; Kučinskas et al. 2013b).
All Tables
All Figures
Fig. 1 3D hydrodynamical CO^{5}BOLD and 1D hydrostatic LHD model atmospheres used in this work, shown in the log g–T_{eff} plane (large yellowfilled circles). Different isochrones (Pietrinferni et al. 2004, 2006) indicate the approximate loci of stars in the Galactic thin and thick disk, bulge, and halo. 

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In the text 
Fig. 2 Comparison of theoretical and observed SEDs of the Sun. Top: solar SEDs computed using 3D hydrodynamical CO^{5} BOLD (green solid line) and 1D LHD (red dotted line) model atmospheres, plotted together with the observed absolute solar flux spectrum from Neckel (1999, black solid line). Bottom: relative differences between the SEDs: observed–3D (black solid line) and 3D–1D (red dashed line, scale on the right yaxis). 

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In the text 
Fig. 3 Comparison of theoretical and observed SEDs of Vega. Top: SEDs of Vega computed using 1D hydrostatic LHD (red dotted line)and ATLAS9 (blue dashed line) model atmospheres, plotted together with the HST CALSPEC absolute calibrated flux spectrum of Vega from the HST CALSPEC library (black solid line). The close overlap of the three lines makes it difficult to distinguish between them. Bottom: relative differences between the SEDs: HST CALSPEC – LHD (red dotted line) and HST CALSPEC – ATLAS9 (blue dashed line). 

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In the text 
Fig. 4 Top: SEDs corresponding to the 3D hydrodynamical CO^{5}BOLD models listed in Table 1. Bottom: relative flux difference between the SEDs computed using 3D hydrodynamical CO^{5} BOLD and 1D hydrostatic LHD model atmospheres. Left panels: [M∕H] = 0.0; right panels: [M∕H] = −2.0. 

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In the text 
Fig. 5 SEDsof the RGB (top row) and TO (bottom row) models computed using 3D hydrodynamical, averaged, and 1D hydrostatic model atmospheres, at [M∕H] = 0.0 (left) and [M∕H] = −2.0 (right). Top panels: SEDs corresponding to different models. Bottom panels: relative differences between the SEDs shown in the corresponding top panels. All SEDs were renormalized to yield the same effective temperature. 

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In the text 
Fig. 6 Relative differences between the SEDs of RGB (top row) and TO (bottom row) stars computed with and without ODFs using 3D hydrodynamical, averaged , and 1D hydrostatic model atmospheres, at [M∕H] = 0.0 (left) and [M∕H] = −2.0 (right). 

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In the text 
Fig. 7 3D–1D magnitude differences in the UBVRIJHK_{s} photometric system computed using 3D hydrodynamical CO^{5}BOLD and 1D hydrostatic LHD models, at [M∕H] = 0.0 and −2.0. 

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In the text 
Fig. 8 Same as Fig. 7, but in the Strømgren photometric system. 

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In the text 
Fig. 9 Differences in the UBVRIJHK_{s} magnitudes obtained from the 1D LHD models that were computed using different mixing length parameters, plotted as differences with respect to the models computed with α_{MLT} = 1.0. Dotted horizontal lines mark zero magnitude differences. The yscale increases downwards and the zero difference lines are shifted incrementally by +0.05 mag from top to bottom. 

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In the text 
Fig. 10 Same as Fig. 9, but for the colour indices. 

Open with DEXTER  
In the text 
Fig. 11 Top: SEDs computed using the original grid of the model atmosphere (kskip = 1) and a coarser grid covering each third cell of the original grid (kskip = 3). A single snapshot of the 3D hydrodynamical model of a red giant was used in the computation of both SEDs. Bottom: differences between the two SEDs shown in the top panel. 

Open with DEXTER  
In the text 
Fig. 12 Effects of opacity binning on the photometric magnitudes in the UBVRIJHK_{s} system. The plot shows differences in the magnitudes of two 3D hydrodynamical CO^{5} BOLD models computed using opacities grouped into 14 and 6 opacity bins. 

Open with DEXTER  
In the text 
Fig. 13 Effects of microturbulence velocity used calculating opacity distribution functions on the spectral energy distribution. The plot shows relative 3D–1D, 3D–<3D>, and <3D>–1D differences in the flux (normalised to that of the corresponding 3D model) of several model atmospheres computed using opacities with microturbulence velocities of 2.0 and 1.0 km s^{−1}. 

Open with DEXTER  
In the text 
Fig. A.1 Flux ratios as predicted the simple model given by Eq. (A.3). For the plot we assumed a temperature fluctuation of σ_{T}∕T = 4%. 

Open with DEXTER  
In the text 
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