Issue 
A&A
Volume 572, December 2014



Article Number  A69  
Number of page(s)  11  
Section  Stellar atmospheres  
DOI  https://doi.org/10.1051/00046361/201424619  
Published online  01 December 2014 
Opacities and spectra of hydrogen atmospheres of moderately magnetized neutron stars^{⋆}
^{1}
Centre de Recherche Astrophysique de Lyon, Université de Lyon, Université
Lyon 1, Observatoire de Lyon, École Normale Supérieure de Lyon, CNRS, UMR
5574,
46 allée d’Italie,
69364
Lyon Cedex 7,
France
^{2}
Ioffe Institute, Politekhnicheskaya 26, 194021
St. Petersburg,
Russia
email:
palex@astro.ioffe.ru
^{3}
Central Astronomical Observatory at Pulkovo,
Pulkovskoe Shosse 65,
196140
Saint Petersburg,
Russia
^{4}
Isaac Newton Institute of Chile, St. Petersburg Branch,
Russia
^{5}
School of Physics, University of Exeter, Exeter, UK,
EX4 4QL,
UK
^{6}
Mathematical Sciences and STAG Research Centre, University of
Southampton, Southampton
SO17 1BJ,
UK
Received: 16 July 2014
Accepted: 26 September 2014
Context. There is observational evidence that central compact objects (CCOs) in supernova remnants have moderately strong magnetic fields B ~ 10^{11} G. Meanwhile, available models of partially ionized hydrogen atmospheres of neutron stars with strong magnetic fields are restricted to B ≳ 10^{12} G. Extension of the applicability range of the photosphere models to lower field strengths is complicated by a stronger asymmetry of decentered atomic states and by the importance of excited bound states.
Aims. We extend the equation of state and radiative opacities, as presented in previous papers for 10^{12}G ≲ B ≲ 10^{15} G, to weaker fields.
Methods. We constructed analytical fitting formulae for binding energies, sizes, and oscillator strengths for different bound states of a hydrogen atom moving in moderately strong magnetic fields and calculate an extensive database for photoionization cross sections of such atoms. Using these atomic data, in the framework of the chemical picture of plasmas we solved the ionization equilibrium problem and calculated thermodynamic functions and basic opacities of partially ionized hydrogen plasmas at these field strengths. Then plasma polarizabilities were calculated from the KramersKronig relation, and the radiative transfer equation for the coupled normal polarization modes was solved to obtain model spectra.
Results. An equation of state and radiative opacities for a partially ionized hydrogen plasma are obtained at magnetic fields B, temperatures T, and densities ρ typical for atmospheres of CCOs and other isolated neutron stars with moderately strong magnetic fields. The first and secondorder thermodynamic functions, monochromatic radiative opacities, and Rosseland mean opacities are calculated and tabulated, considering partial ionization, for 3 × 10^{10}G ≲ B ≲ 10^{12} G, 10^{5} K ≲ T ≲ 10^{7} K, and a wide range of densities. Atmosphere models and spectra are calculated to verify the applicability of the results and to determine the range of magnetic fields and effective temperatures where the incomplete ionization of the hydrogen plasma is important.
Key words: magnetic fields / plasmas / stars: atmospheres / stars: neutron
Tables of thermodynamic functions, atomic number fractions, opacities, and plasma polarizability coefficients are only available at the CDS via anonymous ftp to cdsarc.ustrasbg.fr (130.79.128.5) or via http://cdsarc.ustrasbg.fr/vizbin/qcat?J/A+A/572/A69
© ESO, 2014
1. Introduction
Thermal or thermallike radiation has been detected from several classes of neutron stars, which are characterized by different typical values of magnetic field B. Particularly interesting are isolated neutron stars with clearly observed thermal emission in quiescence, whose thermal Xray spectra formed on the surface are not blended with emission from accreting matter or magnetosphere (see the list of their properties in Viganò et al. 2013). Most of them have surface magnetic fields in the range 10^{12}G ≲ B ≲ 10^{15} G, but one class of sources, so called central compact objects (CCOs) have B ~ afew × (10^{10}−10^{11}) G (Halpern & Gotthelf 2010; Ho 2013). These fields are strong enough to radically affect properties of hydrogen atoms and strongly quantize the electrons in the neutronstar atmosphere, but they are below the field strengths available in the previously developed models of strongly magnetized, partially ionized hydrogen atmospheres of neutron stars, which are currently included in the XSPEC package (Arnaud 1996) under the names NSMAX (Ho et al. 2008) and NSMAXG (Ho 2014). A construction of neutronstar photosphere models for moderately strong magnetic fields has, therefore, become a topical problem. In this paper we construct such models for 3 × 10^{10}<B< 10^{12} G.
We use the theoretical model of a partially ionized hydrogen plasma (Potekhin et al. 1999; hereafter Paper I) that was previously used for opacity calculations at 10^{12} G ≲ B ≲ 10^{15} G (Potekhin & Chabrier 2003, 2004; hereafter Papers II and III, respectively). However, the present task is more arduous, because the field strength is closer to the atomic unit G. Accordingly, the dimensionless magnetic field parameter γ = B/B_{0} is smaller, and the adiabatic approximation for atomic wave functions, which is valid at γ → ∞, becomes less adequate, which entails the need to include more terms than previously in the wavefunction expansion beyond this approximation.
In addition, with decreasing B, the energy spectrum of the bound states of a magnetized atom becomes denser, which necessitates inclusion of more such states in the consideration. Meanwhile, since γ ≫ 1, the centerof mass motion of the atom noticeably affects the atomic properties. In order to cope with the problem, we construct analytical fitting formulae for atomic energies, sizes, and main oscillator strengths as functions of B, discrete quantum numbers of initial and final states, and pseudomomentum K_{⊥}, which corresponds to the state of motion of an atom across the field. These analytical expressions are valid for γ ~ 10–1000 and supplement the previously available fits for larger γ (Potekhin 1998). For boundfree transitions, we calculate extensive tables of cross sections as functions of K_{⊥} and photon frequency ω for a number of bound states at every given B and interpolate across these tables to calculate the opacities in the same way as in Papers II and III.
In Sect. 2 we recall the main properties that characterize the motion of a hydrogen atom in a magnetic field. In Sect. 3 we describe the solution of the ionization equilibrium problem. Section 4 contains the summary of the theoretical methods used to calculate the opacities and polarization vectors of normal electromagnetic modes in a magnetized plasma. Results of numerical calculations are presented and discussed in Sect. 5. In Sect. 6 we formulate conclusions. In the Appendix we present analytical approximations to the results of numerical calculations of the characteristics of a hydrogen atom moving in a strong magnetic field (binding energies, quantummechanical sizes, boundbound transition oscillator strengths) that are used to solve the ionization equilibrium problem and to calculate the opacities.
2. Hydrogen atom in a strong magnetic field
Motion of charged particles in a magnetic field B is quantized in discrete Landau levels. In the nonrelativistic theory, the energy of the Nth Landau level equals Nħω_{ce} (N = 0,1,2,...), where ω_{ce} = eB/m_{e}c is the electron cyclotron frequency. The wave functions that describe an electron in a magnetic field have a characteristic transverse scale of the order of the “magnetic length” , where a_{B} is the Bohr radius.
In a hydrogen atom, the Landau quantization affects motion of both charged particles, electron and proton. For a nonmoving atom in a strong magnetic field, there are two distinct classes of its quantum states: at every value of the Landau quantum number N and the magnetic quantum number − s (N ≥ 0, s ≥ −N), there is one tightly bound state (with “longitudinal” quantum number ν = 0), with binding energy growing asymptotically as (lnγ)^{2}, and an infinite series of looselybound states (ν = 1,2,...) with binding energies below 1 Ry. The sum N + s corresponds to the Landau number for the proton. At B ≳ 10^{9} G, the electronproton binding is possible only for N = 0. Therefore we drop N from the boundstate labeling hereafter. Although the Coulomb interaction mixes different electron and proton Landau orbitals, this numbering is unambiguous and convenient at B ≫ B_{0} (see Potekhin 1994).
Fig. 1
Binding energies of different states (s,ν) of a hydrogen atom as functions of pseudomomentum K_{⊥} at B = 3.16 × 10^{10} G (left), B = 10^{11} G (middle), and B = 10^{12} G (right). Numerical calculations (dots) are compared with the analytical approximation presented in Appendix A.1 (solid lines). For comparison, the fit previously developed for B ≳ 10^{12} G (Potekhin 1998) is shown by the dashed lines in the upper right panel. 

Open with DEXTER 
The binding energy of a hydrogen atom can be written as (1)where so called longitudinal binding energy is positive and corresponds to the relative electronproton motion along B, while the term − ħω_{cp}s diminishes the total binding energy due to transverse quantum excitations by multiples of the proton cyclotron energy ħω_{cp} = ħeB/m_{p}c = 6.305 (B/ 10^{12}G) eV. The atom is elongated: its size along the magnetic field B either decreases logarithmically with increasing γ (for the tightly bound states) or remains nearly constant (for the loosely bound states), while the transverse radius decreases as γ^{− 1/2}.
The astrophysical simulations assume finite temperatures, hence thermal motion of particles. The theory of motion of a system of point charges in a constant magnetic field was reviewed by Johnson et al. (1983). The canonical centerofmass momentum P is not conserved in a magnetic field. A relevant conserved quantity is pseudomomentum, which for the H atom equals K = P − (e/ 2c) B × r, where r connects the proton and the electron. Early studies of the effects of motion were done by Gor’kov & Dzyaloshinskiĭ (1968), Burkova et al. (1976), Ipatova et al. (1984). Vincke & Baye (1988) and Pavlov & Mészáros (1993) developed a perturbation theory for the treatment of atoms moving across the magnetic field at small transverse pseudomomenta K_{⊥}. Numerical calculations of the energy spectrum of the hydrogen atom with an accurate treatment of the effects of motion across a strong magnetic field were performed by Vincke et al. (1992) and Potekhin (1994).
At small K_{⊥} the binding energy is (2)where m_{sν} is an effective “transverse mass”, which is larger than the true atomic mass m_{H}. When K_{⊥} exceeds some critical value K_{c}, the atom becomes decentered. Then the electron and proton are localized near their guiding centers, separated by distance . At K_{⊥} → ∞, . More precisely (Potekhin 1994), (3)where and . The transverse atomic velocity equals ∂E/∂K. Therefore with increasing K_{⊥} the velocity attains a maximum at K_{⊥} = K_{c} and then decreases, while the average electronproton distance continues to increase. For the states with s ≠ 0, E_{sν}(K_{⊥}) can become negative due to the term − ħω_{cp}s in Eq. (1). Such states are metastable. In essence, they are continuum resonances. In the transition region at K_{⊥} ≈ K_{c}, the atomic wave function is a complex superposition of several orbitals, which describe neighboring states outside this region.
The width of the range of K_{⊥} around K_{c}, where the decentering proceeds, decreases with decreasing B. At γ ≳ m_{p}/m_{e} this width is large, and the transition to the decentered state is smooth, but at B ≲ 10^{12} G the width is small compared to K_{c}, so that a tightlybound atom becomes decentered almost abruptly. For this reason, the previous fitting formulae for the K_{⊥}dependences of the binding energies and other characteristics of the H atom were restricted to γ> 300 (Potekhin 1998). In the Appendix we present a new set of fitting formulae, applicable at 10 ≲ γ ≲ 10^{3}. In the overlap region 300 <γ ≲ 10^{3} both sets of fitting expressions describe the atomic characteristics sufficiently well for the use in the opacity modeling.
Figure 1 illustrates the K_{⊥}dependences of binding energies at B = 3.16 × 10^{10} G, B = 10^{11} G, and 10^{12} G. The results of numerical calculations, performed by the method described in Potekhin (1994), are compared with the fitting formulae for 5 lowest tightly bound and 5 lowest loosely bound quantum states. The gaps in the series of calculated points for some states are related to a numerical instability in the transition region around K_{c}, where no single Landau orbital is clearly leading and the energy levels experience anticrossings (see discussion in Potekhin 1994). In these cases the analytical fits are more reliable for calculations of the ionization equilibrium and opacities, which involve integrals over K_{⊥} (see below). In the case of tightly bound states at B = 10^{12} G, the previous fit for γ> 300 (Potekhin 1998) is also shown. Appreciable differences between the two fits are observed only in the transition region K_{⊥} ~ K_{c}, where the anticrossings occur. For the looselybound states, the two fits nearly coincide at this field strength.
3. Ionization equilibrium and equation of state
For photosphere simulations, it is necessary to determine the fractions of different bound states, which affect the spectral features via boundbound and boundfree absorptions. Solution to this problem is laborious and ambiguous. The principal difficulty in the chemical picture of plasmas is the necessity to distinguish the bound and free electrons and “attribute” the bound electrons to certain nuclei (see, e.g., Rogers 2000, and references therein). Current approaches to the solution of this problem are based, as a rule, on the concept of so called occupation probabilities of quantum states. In the case of strong magnetic fields, the occupation probabilities depend not only on the discrete quantum numbers, but also on the transverse pseudomomentum K_{⊥}.
The momentum projections on the magnetic field have the usual Maxwellian distributions at thermodynamic equilibrium for all plasma particles. For transverse motion, however, we have the discrete Boltzmann distribution over Landau numbers for electrons and protons, whereas the transverse momenta of H atoms in a state (s,ν) have a distribution p_{sν}(K_{⊥}), which is not known in advance. We adhere to the definition of p_{sν}(K_{⊥}) in Paper I, so that Ionization equilibrium is given by minimization of the Helmholtz free energy F with respect to particle numbers, keeping volume V and the total number density of protons (free and bound) n_{0} = ρ/m_{H} constant, and the number of electrons equal to that of protons because of the overall electrical neutrality. The free energy is written as (4)where , are the free energies of ideal gases of the electrons and protons, respectively, and F_{ex} takes into account the Coulomb plasma nonideality and the nonideal contribution which arises from interactions of bound species with each other and with the electrons and protons. Finally, F_{at} is the contribution of the atomic gas, including the kinetic and internal degrees of freedom. The formulae for each term in Eq. (4) are given in Papers I and II. In particular, (5)where n_{sν} is the number density of the H atoms with given discrete numbers s and ν (any K_{⊥}), w_{sν}(K_{⊥}) are the occupation probabilities, λ_{H} = [ 2πħ^{2}/ (m_{H}T) ] ^{1/2} is the thermal wavelength of the atom, and (6)is the partition function, which includes the continuous distribution over K_{⊥}. In all mathematical expressions, temperature T is in energy units. As in Paper I, we supplement Eq. (4) by additional terms due to the molecules H_{n} (n ≥ 2) using approximate formulae for the characteristics of H_{n} from Lai (2001). Since the latter do not take full account of the motion effects, the results are reliable only when the abundance of H_{n} is small, which restricts our treatment to T ≳ 10^{5} K.
Fig. 2
Fractional abundances of different nondissolved bound states (s,ν) with respect to the total number of electrons (free and bound), n_{sν}/n_{0}, as functions of mass density ρ, for B = 10^{11} G and T = 2 × 10^{5} K (left panel), B = 10^{11} G and T = 5 × 10^{5} K (middle panel), and B = 10^{12} G and T = 5 × 10^{5} K (right panel). The fractional abundances of tightly bound states (ν = 0) are plotted by dotdashed lines, and loosely bound states (ν ≥ 1) by dashed lines. The solid lines show the total fractional abundance of the atoms that contribute to boundbound and boundfree opacities. 

Open with DEXTER 
Once the free energy is obtained, its derivatives over ρ and T and their combinations provide the other thermodynamic functions. However, the atomic partial number fractions x_{sν} = n_{sν}/n_{0} that are evaluated in the course of the free energy minimization cannot be used directly to calculate opacities. At the considered conditions, interactions between different plasma particles give rise to a significant fraction of clusters. Such clusters contribute to the equation of state similarly to the atoms, lowering the pressure, but their radiationabsorption properties differ from those of an isolated atom. Therefore we should not count them in the fraction of atoms x_{H} that contribute to the boundbound and boundfree opacities. Analogously, at low ρ we should not include in x_{H} the highly excited states that do not satisfy the Inglis & Teller (1939) criterion of spectral line merging, being strongly perturbed by plasma microfields. Such states form the so called optical pseudocontinuum (e.g., Däppen et al. 1987). Thus, we discriminate between the atoms that keep their identity and the “dissolved” states that are strongly perturbed by the plasma environment. This distinction between the “thermodynamic” and “optical” neutral fractions is inevitable in the chemical picture of a plasma (see, e.g., Potekhin 1996, for discussion). The fraction of truly bound atoms is evaluated with the use of the occupation probability formalism. At every s, ν, and K_{⊥}, we calculate the “optical” occupation probability , replacing the InglisTeller criterion by an approximate criterion based on the average atomic size (Eq. (14) of Pavlov & Potekhin 1995). The fraction of weakly perturbed atoms, which contribute to the boundbound and boundfree opacities, constitutes a fraction of the total number of atoms. Here, w_{νs}(K_{⊥}) is the “thermodynamic” occupation probability derived from the free energy, which enters the generalized partition function (6).
Figure 2 illustrates the dependences of the fractional abundances of different weakly perturbed atomic states on ρ, T, and B. The left panel shows the case of B = 10^{11} G and relatively low temperature T = 2 × 10^{5} K. With increasing density, abundance of the bound states first increases at low ρ according to the Saha equation and then decreases at higher ρ because of pressure ionization. The middle panel demonstrates the case of a higher temperature T = 5 × 10^{5} K. In this case, all bound states are less abundant because of the thermal ionization. The right panel demonstrates the case of T = 5 × 10^{5} K and a stronger field, B = 10^{12} G. Here, the abundance of the atoms increases compared to the middle panel because of the larger binding energies. Pressure ionization starts at larger ρ, because the atomic sizes decrease with increasing B. The number of tightly bound states on the right panel is limited to ten (0 ≤ s ≤ 9), the number of states with ν = 1 to two (s = 0,1), and all states with ν ≥ 2 have s = 0, because the states with nonzero s and ν ≥ 2 are merged into continuum at B = 10^{12} G.
4. Polarization modes and opacities
4.1. Polarization modes
Propagation of radiation in magnetized plasmas was discussed in many papers and monographs (e.g., Ginzburg 1970). In coordinates with the zaxis along B, the plasma dielectric tensor is (Ginzburg 1970) (7)where I is the unit tensor, χ = χ^{H} + iχ^{A} is the complex polarizability tensor of plasma, χ^{H} and χ^{A} are its Hermitian and antiHermitian parts, respectively. This tensor becomes diagonal, χ = diag(χ_{+ 1},χ_{1},χ_{0}), in the cyclic (or rotating) coordinates with unit vectors , e_{0} = e_{z}.
At photon energies ħω much higher than (8)where ω_{pl} is the electron plasma frequency and ρ is in g cm^{3}, radiation propagates in the form of extraordinary (hereafter labeled by j = 1) and ordinary (j = 2) normal modes. These modes have different polarization vectors e_{j} and different absorption and scattering coefficients, which depend on the angle θ_{B} between the photon wave vector k and B (e.g., Kaminker et al. 1982). The two modes interact with each other via scattering. Gnedin & Pavlov (1974) formulated the radiative transfer problem in terms of these modes.
At a fixed photon frequency ω, the absorption opacity in each mode j and scattering opacities from mode j into mode j′ can be presented as (e.g., Kaminker et al. 1982) where α = 0, ± 1, e_{j,0} = e_{j,z} and e_{j, ± 1} = (e_{j,x} ± ie_{j,y})/ are the components of e_{j} in the cyclic coordinates. The cross sections σ_{α} depend on ω and α, but not on j or θ_{B}. The total scattering opacity from mode j is , and the total extinction opacity is .
4.2. Scattering
Scattering crosssections in neutronstar photospheres are well known (Ventura 1979; Kaminker et al. 1982; Mészáros 1992). For α = −1, the photonelectron scattering has a resonance at ω_{ce}. Outside a narrow (about the Doppler width) frequency interval around ω_{ce}, the cross sections for the basic polarizations α = 0, ± 1 are (11)where σ_{T} = (8π/ 3)(e^{2}/m_{e}c^{2})^{2} is the nonmagnetic Thomson cross section, and ν_{e,α} are effective damping factors (see below).
The photonion scattering cross section looks analogously, (12)The resonance at ω_{cp} due to the scattering on ions can be important in superstrong fields.
In each case, the damping factor ν_{e,α} or ν_{i,α} is equal to the half of the total rate of spontaneous and collisional decay of the state with energy ħω (see discussion in Potekhin & Lai 2007). The spontaneous decay rates are (13)For the protonelectron plasmas, the damping factors that include the scattering and freefree processes can be approximately written as (Paper II) (14)where is the effective freefree frequency given by Eq. (17) below.
4.3. Absorption
4.3.1. Cyclotron absorption
Without magnetic field, absorption of a photon by a free electron is impossible without involvement of a third particle, which would accept the difference between the values of the total momentum of the electron and the photon before and after the absorption. In a quantizing magnetic field, a photon can be absorbed or emitted by a free electron in a transition between Landau levels. In the nonrelativistic or dipole approximation, such transitions occur between the neighboring levels at the frequency ω_{ce}. In the relativistic theory, the multipole expansion leads to an appearance of cyclotron harmonics (Zheleznyakov 1996). Absorption crosssections at these harmonics were derived in the Born approximation by Pavlov et al. (1980) and represented in a compact form by Suleimanov et al. (2012).
4.3.2. Freefree absorption
The quantization of electron motion gives rise to cyclotron harmonics in the nonrelativistic theory. Pavlov & Panov (1976) derived photon absorption crosssections for an electron, which moves in a magnetic field and interacts with a nonmoving point charge. This model is applicable at ω ≫ ω_{cp}. A more accurate treatment of absorption of a photon by the system of a proton and an electron yields (Paper II; Potekhin 2010) (15)where is an effective photoabsorption collision frequency and is a damping factor. In the electronproton plasma, taking into account the scattering and freefree absorption, we have (Paper II) (16)We see from (15) that and have a resonance at the frequencies ω_{ce} and ω_{cp}, respectively. The effective freefree absorption frequency can be written as (17)where is a dimensionless Coulomb logarithm (, where is a Gaunt factor). Without the magnetic field, is a smooth function of ω. In a quantizing magnetic field, however, it has peaks at the multiples of ω_{ce} and ω_{cp} for all polarizations α. An accurate calculation of (Potekhin 2010) demonstrates that, unlike the electron cyclotron harmonics, the ion cyclotron harmonics are so weak that they can be safely neglected in the neutronstar atmosphere models.
In addition to the freefree absorption due to the electronproton collisions, in Paper II we also considered the freefree absorption due to the protonproton collisions. The results revealed that at T ≲ 10^{7} K and ħω/T ≲ 10 the corresponding photoabsorption cross section is much smaller than the usual freefree absorption due to the protonelectron collisions, whereas at larger ħω it is smaller than the scattering cross section. Therefore the protonproton collisions can be neglected in the opacity calculations.
4.3.3. Boundbound absorption
Fig. 3
Analytical approximations (lines) and results of calculations (symbols) for oscillator strengths of transitions from the ground state to different bound states (s,ν) marked near the respective curves with absorption of a photon with polarization α = −1 (dotdashed lines and empty circles), α = 0 (solid lines and crosses), or α = + 1 (dashed lines and filled dots) at B = 10^{11} G (left panel), 3.16 × 10^{11} G (middle panel), and 10^{12} G (right panel). 

Open with DEXTER 
Boundbound transitions of the H atom moving in a strong magnetic field were studied by Pavlov & Potekhin (1995). In the dipole approximation, the cross section of an atom in a state (s,ν) for absorption of a photon with frequency ω and polarization α with a transition to a state (s′,ν′), averaged over the atomic states of motion, reads (18)where (19)is the normalization integral, (20)is the oscillator strength in the dipole approximation, r_{0} = z, , (21)and φ_{sν;s′ν′}(K_{⊥},Δω) describes a normalized profile of the spectral line at a fixed K_{⊥}, The latter profile is assumed Lorentzian with width Γ_{α;sν;s′ν′}(K_{⊥}), determined by electronatom collisions (see Pavlov & Potekhin 1995). In practice the collisional broadening plays minor role compared to the magnetic broadening due to the dependence of Δω on K_{⊥}, except for stationary frequencies [E_{sν}(K_{⊥}) − E_{s′ν′}(K_{⊥})] /ħ for which dE_{sν}(K_{⊥})/dK_{⊥} = dE_{s′ν′}(K_{⊥})/dK_{⊥} – in particular, [E_{sν}(K_{⊥}) − E_{s′ν′}(K_{⊥})] /ħ at K_{⊥} → 0, (s′ − s)ω_{cp} at K_{⊥} → ∞, and a small frequency corresponding to anticrossings at K_{⊥} ~ K_{c}. The magnetic broadening exceeds by orders of magnitude the usual Doppler broadening, which allows us to neglect the difference between the pseudomomenta in the initial and final states in Eqs. (18) and (20). The spectral profile of the boundbound opacities becomes continuous in a wide frequency range, resembling a reversed boundfree profile. We calculate the integral (18) using analytical approximations for the electron collision widths Γ_{α;sν;s′ν′}(K_{⊥}) suggested in Potekhin (1998) and the approximations for binding energies E_{sν}(K_{⊥}) and oscillator strengths f_{α;sν;s′ν′}(K_{⊥}) presented in the Appendix.
Examples of the oscillator strengths are shown in Fig. 3, where the results of numerical calculations by the method described in Potekhin (1994) are compared with the analytical approximations (Appendix A.3). The figure shows oscillator strengths for the main dipoleallowed transitions from the ground state to excited discrete levels as functions of K_{⊥}. Since the atomic wave functions are symmetric with respect to the zinversion for the states with even ν, and antisymmetric for odd ν, only the transitions that change the parity of ν are allowed for the polarization along the field (α = 0), and only those preserving the parity for the circular polarizations (α = ± 1). For an atom at rest, in the dipole approximation, due to the conservation of the zprojection of the total angular momentum of the system, absorption of a photon with polarization α results in the change of s by α. This selection rule for a nonmoving atom manifests itself in vanishing oscillator strengths at K_{⊥} → 0 for s ≠ α. In an appropriate coordinate system (Burkova et al. 1976; Potekhin 1994), the symmetry is restored at K_{⊥} → ∞, therefore the transition with s = α is the only one that survives also in the limit of large pseudomomenta. But in the intermediate region of K_{⊥}, where the transverse atomic velocity is not small, the cylindrical symmetry is broken, so that transitions to other levels are allowed. For this reason the corresponding oscillator strengths in Fig. 3 have maxima at K_{⊥} ~ K_{c}.
4.3.4. Boundfree absorption
The theory of photoionization of the H atom in a strong magnetic field with allowance for motion and a method of calculation of the cross sections was described by Potekhin & Pavlov (1997), who adapted the Rmatrix formalism (Wigner & Eisenbud 1947; Seaton 1983) to the case under study. Since this numerical treatment is computationally involved, we first compose a set of tables of the photoionization cross sections , and then calculate the boundfree opacities using interpolation across these tables. At a given B, for each of the three basic polarizations α, we calculate on a predefined grid, as in Papers II and III. Now we have refined the grid in photon energy, with log _{10}ħω [ eV ] ranging from 0 to 5 with step 0.01, and modified the grid of log _{10}K_{⊥}. In order to avoid large numerical errors due to strong coupling of the orbitals at K_{⊥} ~ K_{c}, we exclude a range of K_{⊥} around K_{c} and use two separate grids for K_{⊥} below and above the excluded region. Each of these grids has, as previously, an equal step in log K_{⊥}. The size of the excluded region is determined ad hoc, from numerical tests at different K_{⊥} values. The employed modification of the grid is justified by a comparison of the results in the overlap range of B ~ 10^{12} G, which reveals virtually no difference between the opacities calculated with the old and new tables of the boundfree cross sections.
As in Papers II and III, we filter out spurious outliers, which appear because of the BeutlerFano resonances, whose widths are smaller than the step of our grid in log ω, using the 3point median filter at every K_{⊥}. The photoionization threshold is determined independently for every K_{⊥}, using the analytic fits to the binding energies given in Appendix A.1.
In addition to the boundbound and boundfree atomic transitions, in a plasma environment there are transitions from bound states to the highly perturbed atomic states discussed in Sect. 3. These perturbed levels effectively dissolve and merge in a pseudocontinuum, which lies below the photoionization threshold. In order to take into account the radiative transitions into this pseudocontinuum, we employ a technique of belowthreshold extrapolation, which is usual in the zerofield case (Däppen et al. 1987; Stehlé & Jacquemot 1993; Seaton et al. 1994). The details of this technique for the case of an atom moving in a strong magnetic field are given in Paper II. As previously, the precalculated, filtered and extrapolated photoionization cross sections are averaged over K_{⊥} with statistical weights .
4.4. Polarization vectors
In the coordinate system (x′,y′,z′) rotated with respect to (x,y,z) so that z′ is along the wave vector k and B is in the (x′,z′) plane, the electromagnetic polarization vectors e_{j} (Sect. 4.1) can be written as (Ho & Lai 2001, 2003) (22)where Here, the parameters K_{j} and K_{z,j} are expressed in terms of the complex dielectric tensor of a plasma (7), dielectric tensor of vacuum 4πχ^{vac} = diag(a,a,a + q), and the inverse magnetic permeability of the vacuum μ^{1} = I + diag(a,a,a + m). We calculate the plasma dielectric tensor using the relation between the polarizability coefficients χ_{α} and the opacities (Potekhin et al. 2004) (26)The vacuum polarizability and permeability coefficients a, q, and m can be neglected at the relatively weak field strengths considered here, but in general they have been fitted by elementary functions (Potekhin et al. 2004).
5. Atomic signatures in the opacities and spectra
5.1. Basic opacities
Fig. 4
Logarithms of total basic cross sections σ_{α} (solid lines), α = −1,0, + 1 marked “(−)”, “(0)”, and ”(+)”, respectively. For comparison, the logarithms of cross sections without contribution of excited bound states (dotted lines) and freefree cross sections (dashed lines) are plotted. The three panels correspond to three sets of plasma parameters ρ, T, and B marked on the plots. The arrows correspond to different characteristic transition energies for a nonmoving H atom (see text for discussion): 0 – E_{0,0} (the principal photoionization threshold), 1 – (E_{0,0} − E_{1,0}), 1′ – (E_{0,0} − E_{2,0}), 1′′ – (E_{0,0} − E_{3,0}), 2 – (E_{1,0} − E_{2,0}), 2′ – (E_{1,0} − E_{3,0}), 3 – (E_{2,0} − E_{3,0}), 4 – (E_{3,0} − E_{4,0}), 5 – (E_{4,0} − E_{5,0}); 1a – (E_{0,0} − E_{0,1}), 2a – (E_{1,0} − E_{1,1}), 3a – (E_{2,0} − E_{2,1}). The arrows marked c0, c1, c2, c3, c4 correspond to cyclotron harmonics energies (N + 1)ħω_{ce} with N = 0,1,2,3,4, respectively. 

Open with DEXTER 
Figure 4 shows examples of the basic cross sections σ_{α} in Eqs. (9), (10) at T = 3.16 × 10^{5} K and different values of B and ρ. The left panel shows the case of B = 3.16 × 10^{10} G and relatively low density ρ = 10^{3} g cm^{3}. In this case, the number fraction of the atoms is small, x_{H} = 0.0025. Nevertheless, we observe prominent absorption features due to boundbound transitions between the neighboring tightlybound states (s − 1,0) → (s,0), which are allowed in the dipole approximation for α = + 1 for a nonmoving atom. We see also the features corresponding to the transitions (s − 1,0) → (s + 1,0) (s = 1,2), which are dipoleforbidden for an atom at rest but become noticeable for moving atoms. Since the energy difference between the initial and final levels is smaller at K_{⊥} ≠ 0 than at K_{⊥} = 0 (cf. Fig. 1), the maxima of the spectral lines are shifted to the left from the corresponding arrows in the figure, which are plotted at ħω = E_{s + 1,0}(0) − E_{s − 1,0}(0). For the longitudinal polarization α = 0, there are narrow spikes, marked 1a, 2a, 3a, to the left of the energy E_{00}(0), which are due to the transitions from the tightlybound states to the lowest looselybound states of the same smanifold, (s,0) → (s,1), with s = 0,1,2, respectively. At higher energies, we see the peaks that are due to the absorption at the cyclotron fundamental frequency ω_{ce} and its harmonics. The harmonics are not seen, however, in the total cross sections (solid lines in the left panel), because they are dominated by scattering at these energies and plasma parameters.
The quantum cyclotron harmonics become visible in the total cross sections at higher density ρ = 0.1 g cm^{3} (the middle panel), because of the larger freefree absorption. Although the abundance of the atoms is also larger, x_{H} = 0.021, the atomic absorption features are merged into the freefree continuum. The absorption features due to transitions between neighboring tightlybound states reappear at a stronger field B = 3.16 × 10^{11} G (the right panel), partly because of a higher abundance of the atoms (x_{H} = 0.053), but mainly because of the lowering of the continuum level for α = −1 with increasing B. In the latter case, the cyclotronabsorption harmonics are again submerged under the scattering. The signatures of boundbound transitions with absorption of a photon polarized along B (α = 0) are not visible in the middle and right panels, because the looselybound states are destroyed by pressure ionization and form quasicontinuum at this density.
The groundstate photoionization jump above the freefree continuum at ħω = E_{00} is small at B = 3.16 × 10^{10} G in the left panel of Fig. 4 and virtually absent in the middle panel, because the product is smaller than in these cases. However, it is clearly visible at the higher field strength (the right panel). This jump is smoothed by the magnetic broadening and by photoionization of excited tightlybound states, as seen from a comparison with the model where the excited states are neglected, which is plotted by the dotted lines.
Fig. 5
Opacities κ_{j} of the normal polarization modes j = 1,2 (the lower and upper curve of each type, respectively) in a magnetized plasma at ρ = 0.1 g cm^{3} and T = 10^{5.5} K, for B = 10^{11} G and θ_{B} = 10° (left panel), B = 10^{11} G and θ_{B} = 60° (middle panel), and B = 10^{12} G and θ_{B} = 60° (right panel). Accurate opacities (solid lines) are compared with the approximation of the cold, fully ionized plasma (dashed lines). The arrows correspond to different characteristic transition energies and are marked in the same way as in Fig. 4. 

Open with DEXTER 
5.2. Opacities for the normal modes
The basic opacities obtained in Sect. 5.1 have been used to calculate plasma polarizabilities and polarization vectors of the normal modes (Sect. 4.4).
Figure 5 illustrates the effect of incomplete ionization on the opacities for the two normal modes (Sect. 4.1). Here, the atomic features analogous to those in Fig. 4 are also seen. The features marked by numbers 2 through 5 arise from the boundbound radiative transitions from excited tightly bound states, which were not included in the previous opacity calculations (Potekhin et al. 2004). In addition to the boundbound, boundfree, and freefree absorption, we have also included the cyclotron absorption beyond the cold plasma approximation, following Suleimanov et al. (2012). The latter absorption gives rise to the high and narrow peaks, marked “c1” and “c2” in the left and middle panels. These peaks correspond to the synchrotron harmonics (Zheleznyakov 1996) and thus they present a manifestation of an effect of special relativity. For comparison, we plot by dashed lines the opacities calculated in the approximation of cold, fully ionized plasma. In the latter approximation, the atomic features are absent because of the full ionization, and the peaks at the cyclotron harmonics are much smaller. The latter difference demonstrates that, despite the smallness of the relativistic parameters T/m_{e}c^{2} and ħω_{ce}/m_{e}c^{2}, the relativistic effects substantially change the opacities at the cyclotron harmonics frequencies, in agreement Suleimanov et al. (2012).
Figures 4 and 5 show that photoionization becomes substantial at relatively strong magnetic fields. The contribution of the boundbound transitions into the opacities also increases with field increase, but the boundfree absorption grows faster and becomes more important. This tendency continues at higher fields, so that the boundbound transitions becomes unimportant for magnetars, at contrast to the boundfree ones (Paper III).
5.3. Spectra
Fig. 6
Local spectrum of a neutron star with magnetic field B = 10^{11} G, normal to the surface, and with effective temperatures T_{eff} = 10^{6} K, 5 × 10^{5} K, and 2 × 10^{5} K (marked near the curves). The partially ionized atmosphere spectrum (solid lines) is compared with the fully ionized atmosphere model (dashed lines) and with the nonmagnetic atmosphere model (dotted lines). 

Open with DEXTER 
We have included the calculated opacities in the equations of radiative transfer for the two normal modes and solved it numerically with the equations of hydrostatic and energy balance, using the numerical method developed by Ho & Lai (2001). Examples of the resulting atmosphere spectra are shown in Figs. 6 and 7.
Figure 6 shows a spectrum of a neutron star with magnetic field B = 10^{11} G and effective temperatures T_{eff} = 10^{6} K, 5 × 10^{5} K, and 2 × 10^{5} K, calculated using the models of fully and partially ionized hydrogen atmospheres. In these examples, we assumed gravity g = 2 × 10^{14} cm s^{2}, which corresponds, for example, to a neutron star with mass M = 1.4 M_{⊙} and radius R = 10.9 km. For realistic neutronstar equation of state BSk21 (Goriely et al. 2010; Potekhin et al. 2013), this g corresponds to M = 1.8 M_{⊙} and R = 12.5 km. The first and second values of the effective temperatures fall in the range of current observational estimates for a number of thermally emitting neutron stars (Viganò et al. 2013), albeit the hot spots observed on CCOs have T> 10^{6} K. The third value, T_{eff} = 2 × 10^{5} K, has not been observed. Indeed, thermal radiation of such cold neutron star is difficult to measure because of the low thermal flux. However, this value of T_{eff} is also plausible, and if there are such neutron stars at distances within ~100 pc, their thermal spectra may be measured in the future. For the partially ionized models with T_{eff} ≥ 5 × 10^{5} K, one can notice the absorption feature at E = 26 eV, which corresponds to the transition between the ground state and the lowest excited state of the H atom, but otherwise the spectrum is smooth and close to the one in the fully ionized plasma model. The atomic features are rather small and less significant than the cyclotron harmonics. At T_{eff} = 2 × 10^{5} K, more atomic spectral features are discernible. At this field strength, they lie at rather low energies E ≲ 0.1 keV.
Fig. 7
Local spectrum of a partially ionized atmosphere of a neutron star with effective temperature T_{eff} = 5 × 10^{5} K, with magnetic fields B = 3.16 × 10^{11} G (dotdashed line), 10^{11} G (solid line) and 0 G (dotted line). Blackbody spectrum (shortlongdashed line) and spectra of a magnetized, but fully ionized, atmosphere are also shown. 

Open with DEXTER 
Figure 7 presents a comparison of the spectra for B = 10^{11} G and 3.2 × 10^{11} G at T_{eff} = 5 × 10^{5} K, calculated using the models of fully and partially ionized hydrogen atmosphere. At the stronger field, the atomic absorptions make a noticeable contribution to the spectrum at energies ħω ~ 10−100 eV, but even in this case they are not well pronounced. We conclude that the atomic absorption is not very important for the atmosphere spectra at B ≲ 10^{11} G, provided that T_{eff} ≳ 5 × 10^{5} K.
In Figs. 6 and 7 we also show the spectra in the model of partially ionized nonmagnetic H atmosphere (for details of this calculation, see Ho & Heinke 2009). In the latter model, there are no cyclotron lines, atomic absorption features are very weak (barely discernible) because of a high degree of plasma ionization, and the spectral maximum is shifted to higher energies by ~10% compared with the case of B = 10^{11} G. For comparison, in Fig. 7 we plot the blackbody model, which strongly underestimates the peak energy and overestimates the peak flux.
6. Conclusions
We have developed new analytical approximations for energies, sizes, and oscillator strengths of a H atom moving arbitrarily in moderately strong magnetic field 3 × 10^{10} G ≲ B ≲ 10^{12} G. Using these approximations and extensive numerical calculations of the boundfree absorption cross sections, we calculated the ionization equilibrium, equation of state, and opacities at the moderate fields. The tables of the thermodynamic functions, atomic fractions, and Rosseland opacities, previously available online for B = 10^{12}−10^{15} G (Papers I and II), are supplemented by the field interval B = 3 × 10^{10}−10^{12} G.
The calculated spectral opacities are implemented in calculations of the neutronstar atmosphere models. The results show that at B ≪ 10^{12} G and T_{eff} ≳ 5 × 10^{5} K the atomic absorption features in the spectra are small. Boundbound features at such field strengths are more significant than boundfree ones, but they occur at low energies, which are difficult to observe. Moreover, the distribution of the magnetic field over the surface should additionally smear these features and make them less significant, as has been demonstrated in the case of the stronger fields by Ho et al. (2008). On the other hand, despite the smallness of the characteristic thermal and photon energies compared to the electron rest energy, the relativistic cyclotron harmonics are clearly visible in the spectra at these field strengths, in agreement with the results previously reported by Suleimanov et al. (2012) and Ho (2013).
Acknowledgments
The work of AYP on calculation of the opacities and polarizabilities (Sect. 4) has been supported by the Russian Science Foundation (grant 141200316). WCGH appreciates use of computer facilities at KIPAC.
References
 Arnaud, K. A., in Astronomical Data Analysis Software and Systems V, eds. G. Jacoby, & J. Barnes, 1996, ASP Conf. Ser., 101, 17 [NASA ADS] [Google Scholar]
 Burkova, L. A., Dzyaloshinskiĭ, I. E., Drukarev, G. P., & Monozon, B. S. 1976, Sov. Phys. JETP, 44, 276 [NASA ADS] [Google Scholar]
 Däppen, W., Anderson, L., & Mihalas, D. 1987, ApJ, 319, 195 [NASA ADS] [CrossRef] [Google Scholar]
 Ginzburg, V. L. 1970, The Propagation of Electromagnetic Waves in Plasmas, 2nd edn. (London: Pergamon) [Google Scholar]
 Gnedin, Yu. N., & Pavlov, G. G. 1974, Sov. Phys. JETP, 38, 903 [NASA ADS] [Google Scholar]
 Goriely, S., Chamel, N., & Pearson, J. M. 2010, Phys. Rev. C, 82, 035804 [NASA ADS] [CrossRef] [Google Scholar]
 Gor’kov, L. P., & Dzyaloshinskiĭ, I. E. 1968, Sov. Phys. JETP, 26, 449 [NASA ADS] [Google Scholar]
 Halpern, J. P., & Gotthelf, E. V. 2010, ApJ, 709, 436 [NASA ADS] [CrossRef] [Google Scholar]
 Ho, W. C. G. 2013, in Neutron Stars and Pulsars: Challenges and Opportunities after 80 years, ed. J. van Leeuven (Cambridge: Cambridge University Press), Proc., IAU Symp., 291, 101 [Google Scholar]
 Ho, W. C. G. 2014, in Magnetic Fields Throughout Stellar Evolution, eds. M. Jardine, P. Petit, & H. C. Spruit (Cambridge: Cambridge University Press), Proc. IAU Symp., 302, 435 [Google Scholar]
 Ho, W. C. G., & Heinke, C. O. 2009, Nature, 462, 71 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Ho, W. C. G., & Lai, D. 2001, MNRAS, 327, 1081 [NASA ADS] [CrossRef] [Google Scholar]
 Ho, W. C. G., & Lai, D. 2003, MNRAS, 338, 233 [NASA ADS] [CrossRef] [Google Scholar]
 Ho, W. C. G., Potekhin, A. Y., & Chabrier, G. 2008, ApJS, 178, 102 [NASA ADS] [CrossRef] [Google Scholar]
 Inglis, D. R., & Teller, E. 1939, ApJ, 90, 439 [NASA ADS] [CrossRef] [Google Scholar]
 Ipatova, I. P., Maslov, A. Yu., & Subashiev, A. V. 1984, Sov. Phys. JETP, 60, 1037 [Google Scholar]
 Johnson, B. R., Hirschfelder, J. O., & Yang, K. H. 1983, Rev. Mod. Phys., 55, 109 [NASA ADS] [CrossRef] [Google Scholar]
 Kaminker, A. D., Pavlov, G. G., & Shibanov, Yu. A. 1982, Ap&SS, 86, 249 [NASA ADS] [CrossRef] [Google Scholar]
 Lai, D. 2001, Rev. Mod. Phys., 73, 629 [NASA ADS] [CrossRef] [Google Scholar]
 Mészáros, P. 1992, HighEnergy Radiation from Magnetized Neutron Stars (Chicago: University of Chicago Press) [Google Scholar]
 Pavlov, G. G., & Mészáros, P. 1993, ApJ, 416, 752 [NASA ADS] [CrossRef] [Google Scholar]
 Pavlov, G. G., & Panov, A. N. 1976, Sov. Phys. JETP, 44, 300 [NASA ADS] [Google Scholar]
 Pavlov, G. G., & Potekhin, A. Y. 1995, ApJ, 450, 883 [NASA ADS] [CrossRef] [Google Scholar]
 Pavlov, G. G., Shibanov, Yu. A., & Yakovlev, D. G. 1980, Ap&SS, 73, 33–62 [NASA ADS] [CrossRef] [Google Scholar]
 Potekhin, A. Y. 1994, J. Phys. B: At. Mol. Opt. Phys., 27, 1073 [NASA ADS] [CrossRef] [Google Scholar]
 Potekhin, A. Y. 1996, Phys. Plasm., 3, 4156 [CrossRef] [Google Scholar]
 Potekhin, A. Y. 1998, J. Phys. B: At. Mol. Opt. Phys., 31, 49 [NASA ADS] [CrossRef] [Google Scholar]
 Potekhin, A. Y. 2010, A&A, 518, A24 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Potekhin, A. Y. 2014, Phys. Usp., 57, 735 [NASA ADS] [CrossRef] [Google Scholar]
 Potekhin, A. Y., & Chabrier, G. 2003, ApJ, 585, 955 (Paper II) [NASA ADS] [CrossRef] [Google Scholar]
 Potekhin, A. Y., & Chabrier, G. 2004, ApJ, 600, 317 (Paper III) [NASA ADS] [CrossRef] [Google Scholar]
 Potekhin, A. Y., & Lai, D. 2007, MNRAS, 376, 793 [NASA ADS] [CrossRef] [Google Scholar]
 Potekhin, A. Y., & Pavlov, G. G. 1997, ApJ, 483, 414 [NASA ADS] [CrossRef] [Google Scholar]
 Potekhin, A. Y., Chabrier, G., & Shibanov, Yu. A. 1999, Phys. Rev. E, 60, 2193 (Paper I) [NASA ADS] [CrossRef] [Google Scholar]
 Potekhin, A. Y., Lai, D., Chabrier, G., & Ho, W. C. G. 2004, ApJ, 612, 1034 [NASA ADS] [CrossRef] [Google Scholar]
 Potekhin, A. Y., Fantina, A. F., Chamel, N., Pearson, J. M., & Goriely, S. 2013, A&A, 560, A48 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Rogers, F. J. 2000, Phys. Plasm., 7, 51 [NASA ADS] [CrossRef] [Google Scholar]
 Seaton, M. J. 1983, Rep. Progr. Phys., 46, 167 [NASA ADS] [CrossRef] [Google Scholar]
 Seaton, M. J., Yan, Y., Mihalas, D., & Pradhan, A. K. 1994, MNRAS, 266, 805 [NASA ADS] [CrossRef] [Google Scholar]
 Stehlé, C., & Jacquemot, S. 1993, A&A, 271, 348 [NASA ADS] [Google Scholar]
 Suleimanov, V. F., Pavlov, G. G., & Werner, K. 2012, ApJ, 751, 15 [NASA ADS] [CrossRef] [Google Scholar]
 Ventura, J. 1979, Phys. Rev. D, 19, 1684 [NASA ADS] [CrossRef] [Google Scholar]
 Viganò, D., Rea, N., Pons, J. A., Aguilera, D. N., & Miralles, J. A. 2013, MNRAS, 434, 123; online catalog: http://www.neutronstarcooling.info/ [NASA ADS] [CrossRef] [Google Scholar]
 Vincke, M., & Baye, D. 1988, J. Phys. B: At. Mol. Phys., 21, 2407 [NASA ADS] [CrossRef] [Google Scholar]
 Vincke, M., LeDourneuf, M., & Baye, D. 1992, J. Phys. B, 25, 2787 [NASA ADS] [CrossRef] [Google Scholar]
 Wigner, E. P., & Eisenbud, L. 1947, Phys. Rev., 72, 29 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Zheleznyakov, V. V. 1996, Radiation in Astrophysical Plasmas (Dordrecht: Kluwer) [Google Scholar]
Appendix A: Analytical approximations for atomic energies, sizes, and oscillator strengths
Appendix A.1: Binding energies
For the tightly bound states of a nonmoving H atom (any s, ν = 0, K_{⊥} = 0), we use the analytical approximations for binding energies from Potekhin (2014). For the loosely bound states of a nonmoving H atom (ν ≥ 0, K_{⊥} = 0), we use the analytical approximations from Potekhin (1998). Both sets of approximations are valid for many quantum states at γ ≳ 1.
For moving atoms (K_{⊥}> 0) we use different approximations for the centered states, , and decentered states, , and replace the inflection point at K_{c} by the intersection of these two functions. For the centered states, we use Eq. (2) with (A.1)where γ_{sν} and p_{sν} are dimensionless parameters, which are approximated as functions of s and ν: For the decentered states with ν = 0, we use Eq. (3) with (A.2)For the decentered states with ν ≥ 1, we find that the formulae used previously for the binding energies at any K_{⊥} for γ> 300 (Potekhin 1998) remain valid at smaller γ for K_{⊥}>K_{c}.
These approximations are sufficiently accurate for modeling neutron star photospheres. The differences between neighboring energy levels are determined by these formulae with an accuracy of a few percent (except the K_{⊥} ranges near anticrossings) at 10 ≲ γ ≲ 1000. Examples of calculated and fitted binding energies are shown in Fig. 1.
Appendix A.2: Atomic sizes
For the centered states, the electron cloud is cylindrically symmetric at γ ≫ 1, except for the ranges of K_{⊥} near level anticrossings. The rootmeansquare (rms) sizes of this cloud transverse to the magnetic field are (A.3)The atomic size along the field is given at K_{⊥} = 0 by the approximation (Potekhin 1998) This size remains almost constant for the centered states of a moving atom. For the decentered states (K_{⊥}>K_{c}), our approximation of the longitudinal size reads (A.6)Unlike the case of γ> 300 (Potekhin 1998), at smaller γ we do not smooth the transition between Eqs. (A.5) and (A.6).
Although the electron cloud is mostly cylindrically symmetric, the atom is not, because the proton and electron are not centered at the same axis. The atom acquires a constant dipole moment proportional to the mean electronproton separation , which is considerably smaller than r_{∗} for the tightly bound states at K_{⊥}<K_{c} and approaches r_{∗} for the loosely bound or decentered states. At γ ≳ 10, the fractional difference between and r_{∗} can be approximately described by expressions (A.7)Then the total rms size that is used for calculation of the occupation probabilities (Paper I) is given by
Appendix A.3: Oscillator strengths
In this section we present analytical approximations to the oscillator strengths f_{α;sν;s′ν′}(K_{⊥}), discussed in Sect. 4.3.3. It is sufficient to retain only the transitions with ν′ = ν ± 1 for α = 0 and with ν′ = ν for α = ± 1, because the other oscillator strengths are very small due to the smallness of the wavefunction overlap integral implied in the matrix element in Eq. (20). As can be seen in Fig. 2, the looselybound states are populated very weakly compared to the tightly bound states, therefore we can restrict the consideration by initial states with ν = 0. Furthermore, the symmetry relation f_{α;sν;s′ν′} = f_{− α;s′ν′;sν} allows us to consider only the cases where s′ ≥ s. Thus we are left with oscillator strengths for α = ± 1 and for α = 0.
In the dipole approximation for the nonmoving atom, the only nonzero oscillator strengths are those with s′ = s + α. The corresponding oscillator strengths can be approximated as Equation (A.8) reproduces Eq. (21) of Potekhin (1998), but with a fixed typo, and Eq. (A.9) additionally generalizes it to nonzero s.
For the moving atom and α = ± 1, we keep only transitions with Δs = s′ − s< 4, because the oscillator strengths strongly decrease with increasing Δs. First we define a fielddependent characteristic scale of K_{⊥}, (A.10)Then our approximation for the longitudinal polarization reads (A.11)where For the main transition with circular polarization, viz. α = Δs = 1, first we introduce two functions describing at small and large K_{⊥}, respectively, and truncate (replace by 0) the negative values of these functions. At any K_{⊥}, our approximation reads (A.12)where (A.13)The oscillator strengths for the other considered transitions are
All Figures
Fig. 1
Binding energies of different states (s,ν) of a hydrogen atom as functions of pseudomomentum K_{⊥} at B = 3.16 × 10^{10} G (left), B = 10^{11} G (middle), and B = 10^{12} G (right). Numerical calculations (dots) are compared with the analytical approximation presented in Appendix A.1 (solid lines). For comparison, the fit previously developed for B ≳ 10^{12} G (Potekhin 1998) is shown by the dashed lines in the upper right panel. 

Open with DEXTER  
In the text 
Fig. 2
Fractional abundances of different nondissolved bound states (s,ν) with respect to the total number of electrons (free and bound), n_{sν}/n_{0}, as functions of mass density ρ, for B = 10^{11} G and T = 2 × 10^{5} K (left panel), B = 10^{11} G and T = 5 × 10^{5} K (middle panel), and B = 10^{12} G and T = 5 × 10^{5} K (right panel). The fractional abundances of tightly bound states (ν = 0) are plotted by dotdashed lines, and loosely bound states (ν ≥ 1) by dashed lines. The solid lines show the total fractional abundance of the atoms that contribute to boundbound and boundfree opacities. 

Open with DEXTER  
In the text 
Fig. 3
Analytical approximations (lines) and results of calculations (symbols) for oscillator strengths of transitions from the ground state to different bound states (s,ν) marked near the respective curves with absorption of a photon with polarization α = −1 (dotdashed lines and empty circles), α = 0 (solid lines and crosses), or α = + 1 (dashed lines and filled dots) at B = 10^{11} G (left panel), 3.16 × 10^{11} G (middle panel), and 10^{12} G (right panel). 

Open with DEXTER  
In the text 
Fig. 4
Logarithms of total basic cross sections σ_{α} (solid lines), α = −1,0, + 1 marked “(−)”, “(0)”, and ”(+)”, respectively. For comparison, the logarithms of cross sections without contribution of excited bound states (dotted lines) and freefree cross sections (dashed lines) are plotted. The three panels correspond to three sets of plasma parameters ρ, T, and B marked on the plots. The arrows correspond to different characteristic transition energies for a nonmoving H atom (see text for discussion): 0 – E_{0,0} (the principal photoionization threshold), 1 – (E_{0,0} − E_{1,0}), 1′ – (E_{0,0} − E_{2,0}), 1′′ – (E_{0,0} − E_{3,0}), 2 – (E_{1,0} − E_{2,0}), 2′ – (E_{1,0} − E_{3,0}), 3 – (E_{2,0} − E_{3,0}), 4 – (E_{3,0} − E_{4,0}), 5 – (E_{4,0} − E_{5,0}); 1a – (E_{0,0} − E_{0,1}), 2a – (E_{1,0} − E_{1,1}), 3a – (E_{2,0} − E_{2,1}). The arrows marked c0, c1, c2, c3, c4 correspond to cyclotron harmonics energies (N + 1)ħω_{ce} with N = 0,1,2,3,4, respectively. 

Open with DEXTER  
In the text 
Fig. 5
Opacities κ_{j} of the normal polarization modes j = 1,2 (the lower and upper curve of each type, respectively) in a magnetized plasma at ρ = 0.1 g cm^{3} and T = 10^{5.5} K, for B = 10^{11} G and θ_{B} = 10° (left panel), B = 10^{11} G and θ_{B} = 60° (middle panel), and B = 10^{12} G and θ_{B} = 60° (right panel). Accurate opacities (solid lines) are compared with the approximation of the cold, fully ionized plasma (dashed lines). The arrows correspond to different characteristic transition energies and are marked in the same way as in Fig. 4. 

Open with DEXTER  
In the text 
Fig. 6
Local spectrum of a neutron star with magnetic field B = 10^{11} G, normal to the surface, and with effective temperatures T_{eff} = 10^{6} K, 5 × 10^{5} K, and 2 × 10^{5} K (marked near the curves). The partially ionized atmosphere spectrum (solid lines) is compared with the fully ionized atmosphere model (dashed lines) and with the nonmagnetic atmosphere model (dotted lines). 

Open with DEXTER  
In the text 
Fig. 7
Local spectrum of a partially ionized atmosphere of a neutron star with effective temperature T_{eff} = 5 × 10^{5} K, with magnetic fields B = 3.16 × 10^{11} G (dotdashed line), 10^{11} G (solid line) and 0 G (dotted line). Blackbody spectrum (shortlongdashed line) and spectra of a magnetized, but fully ionized, atmosphere are also shown. 

Open with DEXTER  
In the text 
Current usage metrics show cumulative count of Article Views (fulltext article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 4896 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.