Wavelength predictions for the 1s2 2p - 1s2p3p satellite transitions     

Massimo Mazzoni 《Solar physics》1987,108(2):221-225

The energy differences between 1s ²2p 1s2p3p transitions and the corresponding 1s ² 1s3p resonances are expressed by means of a polynomial function of the atomic number. The agreement with experimental data from lithium to potassium is very good. Interpolated values for nitrogen to sodium and argon as well as extrapolation for calcium are reported.  相似文献   

Line intensity ratios of transitions within the 1s 22s 22p 2 ground configuration of Mgvii     

K. M. Aggarwal 《Solar physics》1984,94(1):75-84

Using theR-matrix approach new calculations have been made for the electron impact excitation of the fine structure transitions within the 1s ²2s ²2p ² ground configuration of Mgvii. The computations have been made at a large number of energies in order to account for the contribution of resonances. All partial waves withL 9 are included in the calculations which are considered to be sufficient for the convergence of collision strengths in the energy range below 65 Ry. From this collision strength data, excitation rate coefficients have been calculated at a series of electron temperatures which are employed in the computation of population of the five lowest levels of Mgvii. The line intensity ratios for the transitions³ P ₁ ¹ D ₂ and³ P ₂ ¹ D ₂ to³ P ₁ ¹ S ₀ are then calculated in the temperature range of 10⁵ to 10⁷ K at electron densities in the range 10⁶ to 10¹⁰ cm^–3. The calculated values are in good agreement with the earlier available results.  相似文献   

The 1s 2s states of negative hydrogen     

Claus Ingemann-Hilberg  Mogens Rudkjøbing 《Astrophysics and Space Science》1970,6(1):101-106

Term values for the 1s 2s states of H^– are calculated with the use of simple eigenfunction approximations constructed on the basis of available Hartree-type functions for the 1s ² and 2s ² states of the ion. The results seem to support a tentative identification of the interstellar diffuse absorption bands at 4890 and 6180 as due to negative hydrogen.  相似文献   

X-rays spectroheliograms in lines of Mg xi and Mg xii     

C. Bonnelle  C. Senemaud  G. Senemaud  G. Chambe  M. Guionnet  J. C. Henoux  R. Michard 《Solar physics》1973,29(2):341-355

Spectroheliograms in the L Mg xii line and in the Mg xi resonance (R) 1s ²¹ S ₀-1s2p ¹ P ₁ line, intercombination (I) 1s ²¹ S ₀-1s2p ³ P _1,2, line, and the forbidden (F) 1s ²¹ S ₀-1s2s ³ S ₁ line, have been obtained.Two Bragg crystal spectrometers were used mounted with mechanical collimators to obtain a spatial resolution of 1 × 3. The apparatus was launched on a sounding rocket on July 2nd, 1971. A particularly thorough study was made of the brightest active region (MC 11402).Variations in the F to I Mg xi line intensity ratio from one point to another in the active region did not reveal the presence of high electron densities.The observed intensities of the Mg xi R line, Mg xii L line and Mg x 1s ²2s ² S _1/2-1s2p ¹ P 2s × × ² P1_{1/2, 3/2} S line are not well explained by an isothermal model. Good agreement between computed and observed intensities is obtained using the non-isothermal model proposed here.  相似文献   

Z-dependence of the level intervals in 2s 2 2p 2, 2s 2 2p 3 and 2s 2 2p 4     

Bengt Edĺen 《Solar physics》1972,24(2):356-367

Values of the level intervals in the ground configurations 2s ² 2p ², 2s ² 2p ³ and 2s ² 2p ⁴ have been critically compiled from laboratory observations and from observations of nebular and coronal forbidden transitions. The data are represented within experimental errors by means of semi-empirical extrapolation formulae which contain from 3 to 5 adjusted parameters. The results provide means for checking laboratory and astrophysical identifications and measurements. Tables of best level values are given for the configurations concerned.  相似文献   

Variation in Ovii X-ray line-emission from the solar corona     

H. R. Rugge  A. B. C. Walker Jr. 《Solar physics》1970,15(2):372-379

The variation in intensity of the solar X-ray resonance (1s ^{2 1} S ₀ - 1s2p ¹ P ₁), intercombination (1s ^{2 1} S ₀ - 1s2p ³ P ₁), and forbidden (1s^{2 1} S ₀ - 1s2s ³ P ₁) lines of helium-like Ovii with 2800 MHz solar radio flux is presented for three solar rotations. A high correlation (r 0.80) exists between the intensities of all three X-ray lines and the 2800 MHz solar flux. The ratio of the forbidden to the intercombination line intensities is found to be essentially independent of long term solar activity. This ratio is used to determine upper limits on the coronal electron density and to make inferences concerning the change in density with solar activity.  相似文献   

Forbidden sulphur I lines in the solar spectrum     

J. P. Swings  D. L. Lambert  N. Grevesse 《Solar physics》1969,6(1):3-11

The [SI] lines are due to transitions within the 3s²3p⁴ ground configuration of neutral sulphur. The results are presented from a search for the [Si] lines in the Fraunhofer spectrum. Two identifications are proposed with faint features in the Fraunhofer spectrum: ¹D₂-¹S₀ at = 7725.02 Å and ³P₂-¹D₂ at = 10821.23 Å. Their measured equivalent widths are shown to confirm the value for the solar abundance of sulphur, logN _S = 7.21 (in the scale logN _H = 12.00), which is derived from the permitted high-excitation lines. These lines give the first convincing identification of [Si] lines in an astrophysical source.  相似文献   

S xi Emission Lines in Active Region Spectra Obtained with the Solar euv Rocket Telescope and Spectrograph (Serts)     

Keenan  F.P.  Pinfield  D.J.  Mathioudakis  M.  Aggarwal  K.M.  Thomas  R.J.  Brosius  J.W. 《Solar physics》2000,197(2):253-262

Theoretical electron density sensitive emission line ratios involving a total of eleven 2s ²2p ²–2s2p ³ transitions in Sxi between 187 and 292 Å are presented. A comparison of these with solar active region observations obtained during rocket flights by the Solar EUV Rocket Telescope and Spectrograph (SERTS) reveals generally good agreement between theory and experiment. However, the 186.87 Å line is masked by fairly strong Fexii emission at the same wavelength, while 239.83 Å is blended with an unknown feature, and 285.58 Å is blended with possibly Niv 285.56 Å. In addition, the 191.23 Å line appears to be more seriously blended with an Fexiii feature than previously believed. The presence of several new Sxi lines is confirmed in the SERTS spectra, at wavelengths of 188.66, 247.14 and 291.59 Å, in excellent agreement with laboratory measurements. In particular, the detection of the 2s ²2p ^{2 3} P ₁ –2s2p ^{3 3} P _0,1 transitions at 242.91 Å is the first time (to our knowledge) that this feature has been identified in the solar spectrum. The potential usefulness of the Sxi line ratios as electron density diagnostics for the solar transition region and corona is briefly discussed.  相似文献   

A Comparison of Theoretical mgvi Emission Line Strengths with Active-Region Observations From Serts     

F.P. Keenan  M. Mathioudakis  A.C. Katsiyannis  C.A. Ramsbottom  K.L. Bell  R.J. Thomas  J.W. Brosius 《Solar physics》2002,205(2):265-277

R-matrix calculations of electron impact excitation rates in N-like Mgvi are used to derive theoretical electron-density-sensitive emission line ratios involving 2s ²2p ³–2s2p ⁴transitions in the 269–403 Å wavelength range. A comparison of these with observations of a solar active region, obtained during the 1989 flight of the Solar EUV Rocket Telescope and Spectrograph (SERTS), reveals good agreement between theory and observation for the 2s ²2p ^{3 4} S–2s2p ^{4 4} Ptransitions at 399.28, 400.67, and 403.30 Å, and the 2s ²2p ^{3 2} P–2s2p ^{4 2} Dlines at 387.77 and 387.97 Å. However, intensities for the other lines attributed to Mgvi in this spectrum by various authors do not match the present theoretical predictions. We argue that these discrepancies are not due to errors in the adopted atomic data, as previously suggested, but rather to observational uncertainties or mis-identifications. Some of the features previously identified as Mgvi lines in the SERTS spectrum, such as 291.36 and 293.15 Å, are judged to be noise, while others (including 349.16 Å) appear to be blended.  相似文献   

Transitions in highly ionized silicon     

R. Glass 《Solar physics》1982,80(2):321-331

Configuration interaction wavefunctions are used to calculate energy levels, wavelengths, oscillator strengths, line strengths, transition probabilities, lifetimes and branching ratios for absorption transitions between the 2lnl [n = 2, 3;l l] states for Si xi. Comparison with recent beam-foil experimental data for the 2s2p ¹ P, 2p ^{2 1} D and 2p ^{2 1} S states is generally good, though in some cases cascade effects may be larger than had been expected.  相似文献   

Predicted wavelengths of coronal transitions in the configurations 3s 23p 2, 3s 23p 3 and 3s 23p 4     

Lars Åke Svensson 《Solar physics》1971,18(2):232-243

The level intervals in the ground configurations 3s ²3p ^k(k = 2, 3, 4) have been studied through the isoelectronic sequences up to Ni. Semiempirical expressions for the parameters F ₂(pp) and _p, are derived from observed data and the intervals are recalculated from interpolated or extrapolated values of the parameters. As a result, predicted wavelengths of magnetic-dipole transitions within the configurations are obtained with an estimated uncertainty of one or two Å.  相似文献   

On the excitation of lower levels of singlet helium in quiescent prominences     

N. N. Morozhenko 《Solar physics》1984,92(1-2):153-160

The paper deals with the excitation of the helium singlet level 2¹ P in the homogeneous and filamentary models of quiescent prominences with following parameters: the optical thickness at the limit of helium Lyman continuum _1c ^M = 0.1–100, T _e = 7000 K, n _e = 5 × 10¹⁰ cm^–3. Assuming a model He atom with seven discrete levels (1¹ S, 2³ S, 2¹ S, 2³ P, 2¹ P, 3³ D, 3¹ D) and the continuum the steady state equations for the levels 2³ S, 2¹ P and the continuum have been solved together with the radiative transfer equations for the line 584 Å and the continuum 504 Å. The variations with depth of the functions n ₂ ³ _S /n ₁ ¹ _S (₁ c), n ₂ ¹ _P /n ₁ ¹ _S (_1c ), and n ⁺ _He n _e /n ₁ ¹ S(_1c ) as well as the intensities of the triplet (D₃, 10830 Å) and singlet (16678, 20581 Å) lines have been calculated. Comparison with observations leads to the following conclusions: (1) The line intensities calculated for filamentary models of prominences agree better with observations than those for homogeneous ones. (2) The helium level 2¹ P is excited by diffuse field 584 Å being formed by recombinations and spontaneous transitions 2¹ P – 1¹ S and escaping from the prominence into the space between the filaments and to the surface. (3) Underpopulation of the singlet level 2¹ P may be explained by combination of weak excitation mechanism (recombinations and formation of the diffuse field 584 Å) and strong deexcitation mechanism (spontaneous transitions into the level 1¹ S).  相似文献   

Interplanetary acceleration of energetic particles at 1 and 5 AU     

X. Moussas  J. J. Quenby  J. F. Valdes Galicia 《Astrophysics and Space Science》1982,85(1-2):99-120

Energetic particle (0.1 to 100 MeV protons) acceleration is studied by using high resolution interplanetary magnetic field and plasma measurements at 1 AU (HEOS-2) and at 5 AU (Pioneer 10). Energy changes of a particle population are followed by computing test particle trajectories and the energy changes through the particle interaction with the time varying magnetic field. The results show that considerable particle acceleration takes place throughout the interplanetary medium, both in the corotating interaction regions (CIR) (5 AU), and in quiet regions (1 AU). Although shocks may contribute to acceleration we suggest statistical acceleration within the CIRs is sufficient to explain most energetic particle observations (e.g., McDonaldet al., 1975; Barnes and Simpson, 1976).The first and second order statistical acceleration coefficients which include transit time damping and Alfvén resonance interactions, are found to be well represented byD _T 8.5×10^–6 T ^0.5 MeV s^–1 andD _TT 4×10^–6 T ^1.5 MeV² s^–1 at 5 AU.By comparison, Fisk's estimates (1976), based on quasi-linear theory for transit-time damping, gaveD _TT 5×10^–7 T MeV² s^–1 at 1 AU.  相似文献   

Helium radiation diffusion in prominences     

N. A. Yakovkin  M. Yu. Zeldina  Ch. Lhagvazhav 《Solar physics》1982,81(2):339-354

The following is shown on the basis of a solution of the integral diffusion equations for radiation in a multilevel helium atom under low-temperature plasma conditions (T _e = 7000 K) in the Vertical slab model: (a) Neutral helium is ionized by coronal radiation mainly in the 100–300 Å spectral region; the degree of helium ionization is maximum at the boundary planes, (b) The photorecombinations to the 2³ S and 2¹ S levels and the photoionizations by the Balmer continuum of the Sun are very nearly balanced and this determines the population of these levels. The 2³ S level is destroyed by electron impacts (this reduces the brightness of the triplet lines), and the 2¹ S level decays via the escape of the quanta of 584 through the 2¹ P level, (c) Emission in the resonance line 584 (2¹ P 1¹ S) occurs due to recombination to 2¹ S with subsequent absorption of quanta of infrared radiation 20581. This is a rare case. (d) The radiation of helium is generated in the vicinity of the boundary planes in the region of penetration of radiation with 200 Å, where the density of matter decreases gradually down to the coronal value. In the subordinate lines, the radiation is conditioned by the quasi-resonance scattering of photospheric radiation, (e) The calculated absolute values of the intensities of the helium and hydrogen lines are in good agreement with the observations (see Figure 6).The helium to hydrogen number ratio is close to 0.05.  相似文献   

Extreme Ultraviolet Emission Lines of ca xv in Solar and Laboratory Spectra     

Keenan  F.P.  Aggarwal  K.M.  Katsiyannis  A.C.  Reid  R.H.G. 《Solar physics》2003,217(2):225-233

New R-matrix calculations of electron impact excitation rates in Caxv are used to derive theoretical electron density diagnostic emission line intensity ratios involving 2s ²2p ²–2s2p ³ transitions, specifically R ₁=I(208.70 Å)/I(200.98 Å), R ₂=I(181.91 Å)/I(200.98 Å), and R ₃=I(215.38 Å)/I(200.98 Å), for a range of electron temperatures (T _e=10^6.4–10^6.8 K) and densities (N _e=10⁹–10¹³ cm^–3) appropriate to solar coronal plasmas. Electron densities deduced from the observed values of R ₁, R ₂, and R ₃ for several solar flares, measured from spectra obtained with the Naval Research Laboratory's S082A spectrograph on board Skylab, are found to be consistent. In addition, the derived electron densities are in excellent agreement with those determined from line ratios in Caxvi, which is formed at a similar electron temperature to Caxv. These results provide some experimental verification for the accuracy of the line ratio calculations, and hence the atomic data on which they are based. A set of eight theoretical Caxv line ratios involving 2s ²2p ²–2s2p ³ transitions in the wavelength range 140–216 Å are also found to be in good agreement with those measured from spectra of the TEXT tokamak plasma, for which the electron temperature and density have been independently determined. This provides additional support for the accuracy of the theoretical line ratios and atomic data.  相似文献   

A comparison of theoretical line strengths for the 2s 22p 2 − 2s2p 3 transitions in Ne v with solar data     

F. P. Keenan  K. M. Aggarwal 《Solar physics》1989,122(1):1-6

Results are presented for several theoretical line ratios in Nev involving transitions between multiplets in the 2s ²2p ² and 2s2p ³ configurations. A comparison of these with solar data from the S082A and S-055 instruments on board Skylab reveals generally good agreement between theory and experiment, especially in the case of the high-resolution (S082A) observations. However the 2s ²2p ^{2 1} D – 2s2p ^{3 1} P (365.6 Å) and 2s ²2p ^{2 3}P – 2s2p ^{3 3} S (359 Å) lines appear to be blended, possibly with transitions in Fex and Fexi/Fexiii, respectively. We note that the intensity ratio I(365.6 Å)/I(416.2 Å) should be a valuable calibration check for a high-resolution extreme ultraviolet instrument in the spectral range 360–420 Å.  相似文献   

Observation of possible Fe xvii 2p 53p(1S0)-2p 53s(1 P 1, 3 P 1) transitions in spectra of a solar active region and flare     

S. O. Kastner  W. M. Neupert  M. Swartz 《Solar physics》1975,43(1):111-115

Expected wavelengths and relative intensities are obtained, from calculations of other workers, for the hitherto unobserved transitions 2p ⁵3p(¹ S ₀)-2p ⁵3s(¹ P ₁, ³ P ₁) in Fe xvii. A candidate pair of lines at 197.05 Å and 242.09 Å was found in laboratory spectra and appears to be present in the spectra of a solar active region observed by the OSO-7 Goddard spectroheliograph, and in the spectrum of a Skylab-observed solar flare.  相似文献   

On intensity ratios of helium and hydrogen lines in quiescent prominences     

Morozhenko  N. N. 《Solar physics》1974,34(2):313-322

Observations of the lines He i 3888 and H8 in 80 quiescent prominences by the author, and in other prominences by Kubota et al. (1972) and Morozhenko (1971), have been used to derive the dependences of I(3888)/I(H8) on I(H8), N ₂ ³ _s on ₀ (H), and N ⁺ n _e on ₀(H) (Figures 1, 2, 3 and 4). The equations of ionization equilibrium and triplet system steady state for a helium atom (27 levels and continuum were considered) were solved together with the radiation transfer equation in the helium Lyman continuum. As given n _e () distribution with depth and T _e =7500 K were assumed. The 2³ S level population N₂ ³ s, helium emission measure N ⁺ n _e and the intensity ratios of the He i 3888 and H8 lines were calculated and compared with observation (Figures 2, 3 and 4, solid lines). The figures show that in bright prominences the observed values of N ₂ ³ s and N ⁺ n _e are systematically higher than the calculated ones. These deviations cannot be eliminated by decreasing n _e . One can make the calculations and observations agree for bright prominences by increasing the UV radiation which penetrates into the prominence.  相似文献   

Proton collisional excitation in the ground configuration of Fe+12, II     

Donald A. Landman 《Solar physics》1973,31(1):81-89

Improved values of the proton impact excitation cross sections at coronal energies for all the Fe⁺¹² ground configuration (3s ²3p ²) transitions are presented. These were obtained by direct computer integration of the Schroedinger equation (with the states expressed in intermediate coupling) resulting from the semi-classical Coulomb excitation theory formulation of the process. Comparison is made with previous results. The associated rate constants at coronal temperatures are given and compared with the corresponding electron impact excitation rate constants. Some cross-section values for the Fe⁺¹³ 3s ²3p ² P _1/2² P _3/2 excitation are also presented.  相似文献   

λ 4097.3 Niii emission in the chromospheric spectrum?     

D. L. Lambert 《Solar physics》1971,16(2):336-339

The recent tentative identification of a chromospheric emission line at = 4097.342 Å with the Niii transition 3s ² S _1/2 $#x2212; 3p ² P _3/2 is discussed. It is shown that the observed intensity is inconsistent with the observed flux in the XUV resonance lines and considerably greater than the predicted intensity from the chromosphere-corona transition zone. Microphotometry of a plate shows that the line is a short interval of continuum between absorption lines.  相似文献