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Journal articles on the topic 'Paschen'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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1

Osmokrovic, P., and A. Vasic. "Anomalous Paschen effect." IEEE Transactions on Plasma Science 33, no. 5 (2005): 1672–76. http://dx.doi.org/10.1109/tps.2005.856492.

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2

Iwasaki, Sachio, Makoto Oka, Kei Suzuki, and Tetsuya Yoshida. "Hadronic Paschen–Back effect." Physics Letters B 790 (March 2019): 71–76. http://dx.doi.org/10.1016/j.physletb.2018.10.024.

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3

BURM, K. T. A. L. "Paschen curves for metal plasmas." Journal of Plasma Physics 78, no. 2 (2011): 199–202. http://dx.doi.org/10.1017/s0022377811000572.

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AbstractThe Paschen curve for D.C. electric field-driven sources like conductively coupled plasmas is examined. The considered plasma gases are metals. The minimum breakdown requirement is related to the ionization energy and the collision cross section of the considered plasma. The dominant collisions to consider may depend on the plasma source.

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4

Akers, David. "Paschen-Back effect in dyonium." International Journal of Theoretical Physics 26, no. 5 (1987): 451–54. http://dx.doi.org/10.1007/bf00668777.

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5

Levko, Dmitry, Robert R. Arslanbekov, and Vladimir I. Kolobov. "Modified Paschen curves for pulsed breakdown." Physics of Plasmas 26, no. 6 (2019): 064502. http://dx.doi.org/10.1063/1.5108732.

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6

Lange, C., J. Baldzuhn, S. Fink, R. Heller, M. Hollik, and W. H. Fietz. "Paschen Problems in Large Coil Systems." IEEE Transactions on Applied Superconductivity 22, no. 3 (2012): 9501504. http://dx.doi.org/10.1109/tasc.2011.2179393.

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7

Zentile, Mark A., Rebecca Andrews, Lee Weller, Svenja Knappe, Charles S. Adams, and Ifan G. Hughes. "The hyperfine Paschen–Back Faraday effect." Journal of Physics B: Atomic, Molecular and Optical Physics 47, no. 7 (2014): 075005. http://dx.doi.org/10.1088/0953-4075/47/7/075005.

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8

Torres, C., P. G. Reyes, F. Castillo, and H. Martínez. "Paschen law for argon glow discharge." Journal of Physics: Conference Series 370 (June 19, 2012): 012067. http://dx.doi.org/10.1088/1742-6596/370/1/012067.

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9

Bary, Jeffrey S., and Sean P. Matt. "Measuring the physical conditions of accreting gas in T Tauri systems." Proceedings of the International Astronomical Union 3, S243 (2007): 95–102. http://dx.doi.org/10.1017/s1743921307009453.

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AbstractHydrogen emission lines observed from T Tauri stars (TTS) are associated with the accretion/outflow of gas in these young star forming systems. Magnetospheric accretion models have been moderately successful at reproducing the shapes of several Hi emission line profiles, suggesting that the emission arises in the accretion funnels. Despite considerable effort to model and observe these emission features, the physical conditions of the gas confined to the funnel flows remain poorly constrained by observation. We conducted a mutli-epoch near-infrared spectroscopic survey of 16 actively a

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10

Cidale, L., J. Zorec, J. P. Maillard, and N. Morrell. "Paschen and Brackett Lines in Be stars." International Astronomical Union Colloquium 175 (2000): 472–75. http://dx.doi.org/10.1017/s0252921100056281.

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AbstractThe activities detected in Be stars indicate that the formation of the circumstellar envelope and its structure cannot be studied independently of the phenomena taking place in the outermost layers of the central stars. Assuming that related to the stellar activity there is an expanding atmospheric region with temperatures Te > Teff followed by an envelope with a decreasing temperature, we calculated hydrogen line profiles for different velocity fields and different positions of temperature maxima relative to the underlying photosphere. Results show that the Hα line is not very sens

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11

Stehlé, C. "Paschen lines of hydrogen and He+ion." Physica Scripta T65 (January 1, 1996): 183–87. http://dx.doi.org/10.1088/0031-8949/1996/t65/027.

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12

Fink, S., W. H. Fietz, G. Kraft, H. Scheller, E. Urbach, and V. Zwecker. "Paschen testing of ITER prototype cryogenic axial breaks." Fusion Engineering and Design 88, no. 9-10 (2013): 1475–77. http://dx.doi.org/10.1016/j.fusengdes.2012.11.028.

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13

Shapiro, A. I., D. M. Fluri, S. V. Berdyugina, and J. O. Stenflo. "Molecular Hanle effect in the Paschen-Back regime." Astronomy & Astrophysics 461, no. 1 (2006): 339–49. http://dx.doi.org/10.1051/0004-6361:20066030.

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14

Kurosawa, Ryuichi, Tim J. Harries та Neil H. Symington. "Time-series Paschen-β spectroscopy of SU Aurigae". Monthly Notices of the Royal Astronomical Society 358, № 2 (2005): 671–83. http://dx.doi.org/10.1111/j.1365-2966.2005.08808.x.

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15

Ovsiannikov, V. D., and E. V. Tchaplyguine. "The PaschenBack effect in helium spectra revisited." Canadian Journal of Physics 80, no. 11 (2002): 1383–89. http://dx.doi.org/10.1139/p02-102.

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The complete information for the intensities of the Zeeman components in the helium triplet lines corresponding to the radiation transitions n3 PJM [Formula: see text] n' 3S1M ' is analyzed in the field-strength region from anomalous Zeeman effects to complete PaschenBack effects. The diagonalization of the paramagnetic interaction for n3PJM was carried out for the states with magnetic quantum number M = 0 in the Hilbert space of dimension 3, taking account of all three fine-structure sublevels, J = 0,1,2. The results of the numerical calculations for line positions and intensities are presen

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16

Knaster, J., and R. Penco. "Paschen tests in superconducting coils: why and how." IEEE Transactions on Applied Superconductivity 22, no. 3 (2012): 9002904. http://dx.doi.org/10.1109/tasc.2011.2175475.

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17

McAllister, I. W. "Illusory Paschen curves associated with strongly electronegative gases." IEEE Transactions on Electrical Insulation 26, no. 3 (1991): 391–97. http://dx.doi.org/10.1109/14.85109.

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18

Osmokrovic, P., I. Krivokapic, and S. Krstic. "Mechanism of electrical breakdown left of Paschen minimum." IEEE Transactions on Dielectrics and Electrical Insulation 1, no. 1 (1994): 77–81. http://dx.doi.org/10.1109/94.300234.

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19

Sargsyan, Armen, Grant Hakhumyan, Claude Leroy, Yevgenya Pashayan-Leroy, Aram Papoyan, and David Sarkisyan. "Hyperfine Paschen–Back regime realized in Rb nanocell." Optics Letters 37, no. 8 (2012): 1379. http://dx.doi.org/10.1364/ol.37.001379.

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20

Andrillat, Y. "Near Infrared Spectra of 103 Bright Be Stars." International Astronomical Union Colloquium 92 (August 1987): 237–38. http://dx.doi.org/10.1017/s025292110011629x.

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We have observed 103 bright Be stars in the near infrared up to 10500 A with a dispersion of 230 and 50 A mm-1. The observations were performed with a Reticon (1024 diodes) attached to the ROUCAS spectrograph at the 193 cm telescope of the Haute Provence Observatory.In this spectral range, the Be stars are characterized by the lines of HI (Paschen series), 0I(7772-74-75, 8446 A), CaII(8542, 8662, 8498 A), FeII(7712, 9997 A) and NI(8686-83-80, 8719-12-03, 8629 A).On our spectra, the CaII triplet is always blended with P13, P15, P16, and only the enhancement of these lines permits to conclude to

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21

Bensammar, S., M. Friedjung, N. Letourneur, and J. P. Maillard. "A P Cygni Profile for the He 10830 A line of CI Cyg in Eclipse." International Astronomical Union Colloquium 103 (1988): 193–95. http://dx.doi.org/10.1017/s0252921100103392.

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AbstractInfrared spectroscopic observations of CI Cyg in eclipse show a P Cygni profile for He I 10830 Å, with a wind velocity of the order of 150 km/s, not seen in hydrogen Brackett and Paschen emission lines, which are single peaked.

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22

Falchi, A., R. Falciani, and P. Mauas. "Infrared and Submillimeter Diagnostics of Activity and Flares." Symposium - International Astronomical Union 154 (1994): 113–23. http://dx.doi.org/10.1017/s0074180900124337.

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We give a critical review of the observations of solar activity in the IR and sub-mm range, which are quite scarce, except for the Fe I triplet at 1.56 μm and the Mg I emission lines at 12.32 μm. These, however, are mainly intended for solar magnetic field studies rather than physical diagnostics on activity phenomena. We compute the emission in some continuuum windows and in some detectable Paschen and Brackett lines in two extreme flare models, viz. a “chromospheric” and a white-light flare model. The utility of the Paschen and Brackett lines as diagnostics of the atmospheric state is questi

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23

Linden, Carsten. "Joachim Paschen: Die Weltenlenker. Zur Vorgeschichte des Zweiten Weltkriegs." Das Historisch-Politische Buch 67, no. 2 (2019): 217. http://dx.doi.org/10.3790/hpb.67.2.217a.

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24

Alexander, D. M., S. Young, and J. H. Hough. "Polarized broad HeI and Paschen lines in NGC 1068." Monthly Notices of the Royal Astronomical Society 304, no. 1 (1999): L1—L4. http://dx.doi.org/10.1046/j.1365-8711.1999.02417.x.

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25

Huang, W., G. Wallerstein, and M. Stone. "A catalogue of Paschen-line profiles in standard stars." Astronomy & Astrophysics 547 (October 29, 2012): A62. http://dx.doi.org/10.1051/0004-6361/201219804.

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26

Cohen, Jeffrey M., and Boris Kuharetz. "SS433 and hydrogen spectrum beyond the Paschen-Back region." International Journal of Theoretical Physics 31, no. 7 (1992): 1197–201. http://dx.doi.org/10.1007/bf00673920.

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27

Lee, S. M., Y. S. Seo, and J. K. Lee. "Paschen breakdown curve by one-dimensional PIC-MCC simulation." Computer Physics Communications 177, no. 1-2 (2007): 132. http://dx.doi.org/10.1016/j.cpc.2007.02.057.

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28

Druett, M. K., and V. V. Zharkova. "HYDRO2GEN: Non-thermal hydrogen Balmer and Paschen emission in solar flares generated by electron beams." Astronomy & Astrophysics 610 (February 2018): A68. http://dx.doi.org/10.1051/0004-6361/201731053.

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Aim. Sharp rises of hard X-ray (HXR) emission accompanied by Hα line profiles with strong red-shifts up to 4 Å from the central wavelength, often observed at the onset of flares with the Specola Solare Ticinese Telescope (STT) and the Swedish Solar Telescope (SST), are not fully explained by existing radiative models. Moreover, observations of white light (WL) and Balmer continuum emission with the Interface Region Imaging Spectrograph (IRISH) reveal strong co-temporal enhancements and are often nearly co-spatial with HXR emission. These effects indicate a fast effective source of excitation a

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29

Kuznetsova, T. N. "Absorption Lines of Call and H in the Near IR Region of the Magnetic Star HD 152107." International Astronomical Union Colloquium 90 (1986): 323–26. http://dx.doi.org/10.1017/s0252921100091739.

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AbstractA behaviour of H lines P12 - P13 and CaII triplet of the star HD 152107 is studied in the range λλ 8400 - 8800 Å. An analysis of the obtained data enabled us to suspect the presence of a relationship between the variation of equivalent widths of the lines of the Paschen series of Hydrogen CaII lines and that of the star’s magnetic field.

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30

Iwasaki, Sachio, Makoto Oka, Kei Suzuki, and Tetsuya Yoshida. "Hadronic Paschen-Back effect in P-wave charmonia under strong magnetic fields." International Journal of Modern Physics: Conference Series 49 (January 2019): 1960002. http://dx.doi.org/10.1142/s2010194519600024.

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The Hadronic Paschen-Back effect (HPBE) is a new phenomenon induced by the interplay between finite orbital angular momenta of hadrons and external strong magnetic fields. We review the HPBE in P-wave charmonia and show its mass spectra, deformed wave functions, and mixing ratios, which are evaluated by the constituent quark models in a magnetic field and the cylindrical Gaussian expansion method.

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31

Bezrukov, Andrei, and Igor Zarubin. "METHODS FOR IMPROVEMENT OF HIGH-RESOLUTION SPECTROMETER CHARACTERISTICS." Interexpo GEO-Siberia 8 (2019): 226–37. http://dx.doi.org/10.33764/2618-981x-2019-8-226-237.

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The present paper demonstrates results of high-resolution spectrometer characteristics improvement methods. Increasing resolution, spectral range extending and illumination efficiency for the spectrometer were investigated. Obtained results will be found useful in atomic spectroscopy applications such as atomic absorption, atomic emission spectroscopy, mass-spectroscopy, chromatography and others. In order to increase spectrometer resolution it was suggested to use higher diffractive grating curvature radius. Experimentally, characteristics of both spectrometer prototypes assembled using diffr

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32

Sowmya, K., K. N. Nagendra, M. Sampoorna, and J. O. Stenflo. "Paschen-Back effect involving atomic fine and hyperfine structure states." Proceedings of the International Astronomical Union 10, S305 (2014): 154–58. http://dx.doi.org/10.1017/s1743921315004688.

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AbstractThe linear polarization in spectral lines produced by coherent scattering is significantly modified by the quantum interference between the atomic states in the presence of a magnetic field. When magnetic fields produce a splitting which is of the order of or greater than the fine or hyperfine structure splittings, we enter the Paschen-Back effect (PBE) regime, in which the magnetic field dependence of the Zeeman splittings and transition amplitudes becomes non-linear. In general, PBE occurs for sufficiently strong fields when the fine structure states are involved and for weak fields

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33

Wang, Q. D., H. Dong, A. Cotera та ін. "HST/NICMOS Paschen-α Survey of the Galactic Centre: Overview". Monthly Notices of the Royal Astronomical Society 402, № 2 (2010): 895–902. http://dx.doi.org/10.1111/j.1365-2966.2009.15973.x.

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34

Straižys, V. "Synthetic Photometry Experiments in the Vicinity of the Paschen Jump." Open Astronomy 7, no. 4 (1998): 571–88. http://dx.doi.org/10.1515/astro-1998-0404.

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35

Xiongyi Huang, Yuntao Song, Kun Lu, et al. "High Voltage Test of ITER Feeder Components Under Paschen Condition." IEEE Transactions on Applied Superconductivity 22, no. 3 (2012): 7701004. http://dx.doi.org/10.1109/tasc.2011.2180292.

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36

Fremat, Y., L. Houziaux, and Y. Andrillat. "Higher Paschen lines in the spectra of early-type stars." Monthly Notices of the Royal Astronomical Society 279, no. 1 (1996): 25–31. http://dx.doi.org/10.1093/mnras/279.1.25.

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37

Heylen, A. E. D. "Sparking formulae for very high-voltage Paschen characteristics of gases." IEEE Electrical Insulation Magazine 22, no. 3 (2006): 25–35. http://dx.doi.org/10.1109/mei.2006.1639027.

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38

Zheng, Jinxing, Yuntao Song, Xiongyi Huang, et al. "Experimental Study on Paschen Tests of ITER Current Lead Insulation." Plasma Science and Technology 15, no. 2 (2013): 152–56. http://dx.doi.org/10.1088/1009-0630/15/2/15.

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39

Radovic, M. K., and D. A. Bosan. "Long formative time lags in nitrogen below the Paschen minimum." Journal of Physics D: Applied Physics 20, no. 5 (1987): 639–41. http://dx.doi.org/10.1088/0022-3727/20/5/012.

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40

Heilger, Marian. "Harm Paschen/Lothar Wigger: Zur Analysepädagogischer Argumentationen. Berichtdes Forschungsprojektes „Bielefelder Katalogpädagogischer Argumente”. Weinheim1992. 130 Seiten.Harm Paschen/Lothar Wigger (Hrsg.):Pädagogisches Argumentieren. Weinheim1992. 395 Seiten." Vierteljahrsschrift für wissenschaftliche Pädagogik 73, no. 4 (1997): 507–8. http://dx.doi.org/10.30965/25890581-07304011.

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41

Munari, Ulisse. "Far-Red Spectroscopy of Peculiar Stars and the GAIA Mission." International Astronomical Union Colloquium 187 (2002): 25–30. http://dx.doi.org/10.1017/s0252921100001184.

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AbstractThe coming GAIA Cornerstone mission by ESA will provide micro-arcsec astrometry, ∼10 bands photometry and far-red spectroscopy for a huge number of stars in the Galaxy (109). GAIA spectroscopy will cover the range 8480–8740 Å which includes the CaII triplet and the head of the Paschen series. In this paper we address the diagnostic potential of this wavelength range toward detection of peculiar stars.

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42

Radwan, Samah, H. El-Khabeary, and A. Helal. "Verification of Paschen Law using a Mixed Geometry Disc-Conical Electrodes." Journal of Engineering Science and Military Technologies 17, no. 17 (2017): 1–10. http://dx.doi.org/10.21608/ejmtc.2017.21230.

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43

Lee, Min Uk, Jimo Lee, Jae Koo Lee, and Gunsu S. Yun. "Extended scaling and Paschen law for micro-sized radiofrequency plasma breakdown." Plasma Sources Science and Technology 26, no. 3 (2017): 034003. http://dx.doi.org/10.1088/1361-6595/aa52a8.

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44

Rudy, Richard J., R. C. Puetter, and S. Mazuk. "Paschen Lines and the Reddening of the Radio Galaxy 3C 109." Astronomical Journal 118, no. 2 (1999): 666–69. http://dx.doi.org/10.1086/300980.

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45

Falceta-Gonçalves, D., та Z. Abraham. "Constraining the orbital orientation of η Carinae from H Paschen lines". Monthly Notices of the Royal Astronomical Society 399, № 3 (2009): 1441–46. http://dx.doi.org/10.1111/j.1365-2966.2009.15364.x.

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46

Lilly, S. J., and G. J. Hill. "The reddening of Cygnus A from a measurement of Paschen-Alpha." Astrophysical Journal 315 (April 1987): L103. http://dx.doi.org/10.1086/184869.

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47

Radwan, Samah, H. El-Khabeary, and A. Helal. "Verification of Paschen Law using a Mixed Geometry Disc-Conical Electrodes." International Conference on Aerospace Sciences and Aviation Technology 17, AEROSPACE SCIENCES (2017): 1–10. http://dx.doi.org/10.21608/asat.2017.22465.

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48

Burm, K. T. A. L. "Calculation of the Townsend Discharge Coefficients and the Paschen Curve Coefficients." Contributions to Plasma Physics 47, no. 3 (2007): 177–82. http://dx.doi.org/10.1002/ctpp.200710025.

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49

Poszwa, A., and A. Rutkowski. "Relativistic Paschen-Back Effect for the Two-Dimensional H-Like Atoms." Acta Physica Polonica A 117, no. 3 (2010): 439–44. http://dx.doi.org/10.12693/aphyspola.117.439.

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50

Taylor, Andrew S., and Oleg V. Batishchev. "Experimental measurements of the Paschen–Back effect in helium triplet transitions." Canadian Journal of Physics 95, no. 10 (2017): 993–98. http://dx.doi.org/10.1139/cjp-2016-0965.

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Experimental confirmation of the theoretical calculations of the Zeeman and Paschen–Back effects in the prominent 2 3S – 2 3P He I 1083 nm near-infrared (NIR) transition by means of high-resolution spectroscopy is reported. A novel approach using a small-pixel-size fluorescence camera delivers required spectral resolution. In particular, it allows to quantify with good precision the spectral shift of the weak λ0 = 1082.9 nm line from the zero magnetic field position. Measurements of the strong visible (VIS) He I 587 and 706 nm triplet line shapes are reported for B = 0–1.0 T interval, indicati

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