The East-West Asymmetry of Cosmic Radiation at a Geomagnetic Latitude of 28°31′ and an Estimation of the Difference of the Exponents of the Absorption Law for the Polar and the Equatorial Regions

1946 ◽  
Vol 69 (9-10) ◽  
pp. 531-531
Author(s):  
Francis Oster ◽  
Sheng-Lin Ch'u ◽  
Lieh-Yang Lü
Keyword(s):  
Cosmic Radiation ◽  
Geomagnetic Latitude ◽  
The Difference ◽  
Absorption Law ◽  
East West

scholarly journals Momentum Distribution and Charge Ratio of µ?Mesons at Zenith Angles in the East?West Plane

1954 ◽  
Vol 7 (3) ◽  
pp. 423 ◽  
Author(s):  
JR Moroney ◽  
JK Parry
Keyword(s):  
Sea Level ◽  
Momentum Distribution ◽  
Cosmic Radiation ◽  
Geomagnetic Latitude ◽  
Vertical Direction ◽  
Charge Ratio ◽  
Momentum Range ◽  
East West

The momentum distribution and charge ratio of the penetrating component of the cosmic radiation at sea-level have been determined over the 'momentum range- 0�24-58 BeVlc at a geomagnetic latitude of 47 oS. The measurements were performed in the vertical direction and at zenith angles of 30� and 60� in the eastern and western azimuths.

scholarly journals The search of the anisotropy of the primary cosmic radiation by the difference method

2017 ◽  
Vol 145 ◽  
pp. 03003
Author(s):  
Victor Pavlyuchenko ◽  
Romen Martirosov ◽  
Natalia Nikolskaya ◽  
Anatoly Erlykin
Keyword(s):  
Difference Method ◽  
Cosmic Radiation ◽  
Primary Cosmic Radiation ◽  
The Difference

scholarly journals Efektifitas Pembayangan yang dihasilkan Pohon dan Bangunan di Koridor Jalan Perkotaan Untuk Mencapai Kenyamanan Termal

2018 ◽  
Vol 4 (1) ◽  
pp. 65-70
Author(s):  
Jockie Zudhy Fibrianto ◽  
Mochamad Hilmy
Keyword(s):  
Thermal Comfort ◽  
Temperature Difference ◽  
Weather Conditions ◽  
The Sun ◽  
The Road ◽  
Analysis Phase ◽  
Measurement Results ◽  
The Difference ◽  
Road Corridors ◽  
East West

The road corridor in Pontianak City has different shading output depending on the sun orientation. The difference has caused a temperature difference that affects the pedestrian thermal comfort along the corridor. Identification and measurement of shading temperatures that occur due to buildings and trees were carried out for three days in each afternoon with relatively similar weather conditions. The road corridor that becomes the research location was at A. Yani St.-Gajah Mada St.-Tanjung Pura St., which has a North-South orientation and Teuku Umar St.-Diponegoro St.-Sisingamangaraja St., who has an East-West direction. The analysis phase is done by comparing the effectiveness of imagery produced by buildings and trees. After that, the identification and measurement results are compared with Indonesian thermal comfort standards SNI T-14-1993-03 to obtain suitable thermal comfort in the road corridors in Pontianak City.

THE HYDROGEN COMPONENT IN THE PRIMARY COSMIC RADIATION

1962 ◽  
Vol 40 (9) ◽  
pp. 1049-1055 ◽  
Author(s):  
H. H. Aly
Keyword(s):  
High Altitude ◽  
Cosmic Radiation ◽  
Nuclear Emulsion ◽  
Geomagnetic Latitude ◽  
The Other ◽  
Primary Cosmic Radiation ◽  
Good Agreement

Two values for the flux of the hydrogen component in the primary cosmic radiation have been measured. The first one was over Guam in the Marianas Islands, geomagnetic latitude λ = 0°. The value of the flux was found to be (123 ± 12) hydrogen nuclei/m2 sterad sec. The second measurement was made over Texas, λ = 41 °N., and the value found was (530 ± 53) hydrogen nuclei/m2 sterad sec. The detectors in both cases were stacks of nuclear emulsion exposed at high altitude. The results obtained in this experiment are in good agreement with the values obtained by the other authors using electronic counters flown at the same geomagnetic latitudes.

FURTHER OBSERVATIONS OF THE HORIZONTAL MOVEMENTS OF AURORA

1960 ◽  
Vol 38 (10) ◽  
pp. 1366-1375 ◽  
Author(s):  
J. A. Kim ◽  
B. W. Currie
Keyword(s):  
Magnetic Field ◽  
Seasonal Variation ◽  
Magnetic Field Intensity ◽  
Geomagnetic Latitude ◽  
Auroral Zone ◽  
The North ◽  
Significant Seasonal Variation ◽  
Positive Correlations ◽  
The Magnetic Field ◽  
East West

A previous paper showed that systematic motions of aurora parallel and normal to the geomagnetic meridians could be deduced from successions of all-sky camera photographs. More reliable deductions which are based on a much larger number of observations, including some from a station inside the auroral zone, are reported in this paper. Both southward and northward speeds increase with geomagnetic latitude to the auroral zone where they become constant, or even decrease slightly, before continuing to increase inside the auroral zone. A seasonal variation of north–south speeds does not appear to exist. A diurnal variation of north–south speeds, dependent on geomagnetic latitude, is evident, the speeds decreasing to a minimum during the morning hours to the south of the auroral zone and increasing to a maximum during the same hours to the north of the zone. Large positive correlations exist between north–south speeds and departures of the magnetic field intensity from normal. East–west speeds either decrease or remain constant with increasing geomagnetic latitude. A significant seasonal variation of east–west speeds is not evident. Eastward speeds are at a maximum between 03 and 04 hours L.M.T., and are associated with negative magnetic bays; westward speeds, between 21 and 22 hours L.M.T., and are associated with positive magnetic bays.

The East-West Asymmetry of the Cosmic Radiation at Very High Elevations Near the Equator

1939 ◽  
Vol 55 (5) ◽  
pp. 503-503 ◽  
Author(s):  
T. H. Johnson ◽  
J. G. Barry
Keyword(s):  
Cosmic Radiation ◽  
High Elevations ◽  
Very High ◽  
East West

scholarly journals <i>F</i>-region ionospheric perturbations in the low-latitude ionosphere during the geomagnetic storm of 25-27 August 1987

2004 ◽  
Vol 22 (10) ◽  
pp. 3479-3501 ◽  
Author(s):  
A. V. Pavlov ◽  
S. Fukao ◽  
S. Kawamura
Keyword(s):  
Geomagnetic Latitude ◽  
Significant Inhibition ◽  
Geomagnetic Equator ◽  
Equatorial Anomaly ◽  
Plasma Drift ◽  
The North ◽  
Mu Radar ◽  
The Difference ◽  
Time Changes ◽  
South Asymmetry

Abstract. We have presented a comparison between the modeled NmF2 and hmF2, and NmF2 and hmF2 which were observed at the equatorial anomaly crest and close to the geomagnetic equator simultaneously by the Akita, Kokubunji, Yamagawa, Okinawa, Manila, Vanimo, and Darwin ionospheric sounders and by the middle and upper atmosphere (MU) radar (34.85° N, 136.10° E) during the 25-27 August 1987 geomagnetically storm-time period at low solar activity near 201°, geomagnetic longitude. A comparison between the electron and ion temperatures measured by the MU radar and those produced by the model of the ionosphere and plasmasphere is presented. The corrections of the storm-time zonal electric field, EΛ, from 16:30 UT to 21:00 UT on 25 August bring the modeled and measured hmF2 into reasonable agreement. In both hemispheres, the meridional neutral wind, W, taken from the HWW90 wind model and the NRLMSISE-00 neutral temperature, Tn, and densities are corrected so that the model results agree with the ionospheric sounders and MU radar observations. The geomagnetic latitude variations in NmF2 on 26 August differ significantly from those on 25 and 27 August. The equatorial plasma fountain undergoes significant inhibition on 26 August. This suppression of the equatorial anomaly on 26 August is not due to a reduction in the meridional component of the plasma drift perpendicular to the geomagnetic field direction, but is due to the action of storm-time changes in neutral winds and densities on the plasma fountain process. The asymmetry in W determines most of the north-south asymmetry in hmF2 and NmF2 on 25 and 27 August between about 01:00-01:30 UT and about 14:00 UT when the equatorial anomaly exists in the ionosphere, while asymmetries in W, Tn, and neutral densities relative to the geomagnetic equator are responsible for the north-south asymmetry in NmF2 and hmF2 on 26 August. A theory of the primary mechanisms causing the morning and evening peaks in the electron temperature, Te, is developed. An appearance, magnitude variations, latitude variations, and a disappearance of the morning Te peaks during 25-27 August are caused by variations in EΛ, thermospheric composition, Tn, and W. The magnitude of the evening Te peak and its time location are decreased with the lowering of the geomagnetic latitude due to the weakening of the effect of the plasma drift caused by W on the electron density. The difference between 25 August and 26-27 August in an appearance, magnitude and latitude variations, and a disappearance of the evening Te peak is caused by variations in W, the thermospheric composition, Tn, and EΛ.

scholarly journals Pulsations, eruptions, and evolution of four yellow hypergiants

2019 ◽  
Vol 631 ◽  
pp. A48 ◽  
Author(s):  
A. M. van Genderen ◽  
A. Lobel ◽  
H. Nieuwenhuijzen ◽  
G. W. Henry ◽  
C. de Jager ◽  
...  
Keyword(s):  
Mass Loss ◽  
Photometric Data ◽  
Data Sets ◽  
Eruptive Episode ◽  
Polycyclic Aromatic ◽  
The Difference ◽  
Stellar Oscillation ◽  
Stellar Properties ◽  
Absorption Law

Aims. We aim to explore the variable photometric and stellar properties of four yellow hypergiants (YHGs), HR 8752, HR 5171A, ρ Cas, and HD 179821, and their pulsations of hundreds of days, and long-term variations (LTVs) of years. We also aim to explore light and colour curves for characteristics betraying evolutionary loops and eruptive episodes and to investigate trends of quasi-periods and the possible need for distance revisions. Methods. We tackled multi-colour and visual photometric data sets, looked for photometric indications betraying eruptions or enhanced mass-loss episodes, calculated stellar properties mainly using a previously published temperature calibration, and investigated the nature of LTVs and their influence on quasi-periods and stellar properties. Results. Based on driven one-zone stellar oscillation models, the pulsations can be characterised as “weakly chaotic”. The BV photometry revealed a high-opacity layer in the atmospheres. When the temperature rises the mass loss increases as well, consequently, as the density of the high-opacity layer. As a result, the absorption in B and V grow. The absorption in B, presumably of the order of one to a few 0.m 1, is always higher than in V. This difference renders redder and variable (B − V) colour indexes, but the absorption law is unknown. This property of YHGs is unpredictable and explains why spectroscopic temperatures (reddening independent) are always higher than photometric ones, but the difference decreases with the temperature. A new (weak) eruption of ρ Cas has been identified. We propose shorter distances for ρ Cas and HR 5171A than the accepted ones. Therefore, a correction to decrease the blue luminescence of HR 5171A by polycyclic aromatic hydrocarbon (PAH) molecules is necessary, and HR 5171A would no longer be a member of the cluster Gum48d. HR 5171A is only subject to one source of light variation, not by two as the literature suggests. Eruptive episodes (lasting one to two years), of YHGs prefer relatively cool circumstances when a red evolutionary loop (RL) has shifted the star to the red on the HR diagram. After the eruption, a blue loop evolution (BL) is triggered lasting one to a few decades. We claim that in addition to HR 8752, also the other three YHGs have shown similar cycles over the last 70 years. This supports the suspicion that HD 179821 might be a YHG (with a possible eruptive episode between 1925 and 1960). The range in temperature of these cyclic Teff variations is 3000 K–4000 K. LTVs mainly consist of such BL and RL evolutions, which are responsible for a decrease and increase, respectively, of the quasi-periods. The reddening episode of HR 5171A between 1960 and 1974 was most likely due to a red loop evolution, and the reddening after the 1975 eruption was likely due to a shell ejection, taking place simultaneously with a blue loop evolution.

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