The Current Solar Minimum and Its Consequences for Climate

Total Page:16

File Type:pdf, Size:1020Kb

The Current Solar Minimum and Its Consequences for Climate Chapter 11 The Current Solar Minimum and Its Consequences for Climate David Archibald Summa Development Limited Chapter Outline 1. Introduction 277 2. The Current Minimum 278 3. Summary 287 1. INTRODUCTION A number of cycles in solar activity have been recognized, including the Schwabe (11 years), Hale (22 years), Gleissberg (88 years), de Vries (210 years), and Bond (1,470 years) cycles. There is nothing to suggest that cyclic behavior in solar activity has ceased for any reason. Therefore, predicting when the next minimum should occur should be as simple as counting forward from the last one. The last major minimum, the Dalton Minimum from 1798 to 1822, was two solar cycles long e Solar Cycles 5 and 6. Recent Gleissberg minima appear to be the decade 1690e1700, Solar Cycle 13 from 1889 to 1901, and Solar Cycle 20 from 1964 to 1976. A de Vries cycle event, herein termed the Eddy Minimum, has started exactly 210 years after the start of the Dalton Minimum. Friis-Christensen and Lassen theory, using methodology pioneered by Butler and Johhnson at Armagh, can be used to predict the temperature response to the Eddy Minimum for individual climate stations with a high degree of confidence. The latitude of the US-Canadian border is expected to lose a month from its growing season with the potential for un-seasonal frosts to further reduce agricultural productivity. Evidence-Based Climate Science. DOI: 10.1016/B978-0-12-385956-3.10011-7 Copyright Ó 2011 Elsevier Inc. All rights reserved. 277 278 PART j IV Solar Activity 2. THE CURRENT MINIMUM As recently as 2008, there was a wide range in estimated amplitudes for Solar Cycle 24, from Dikpati at 190 and Hathaway at 170 respectively to Clilverd (2005) at 42 and Badalyan et al. (2001) at 50. This enormous divergence in projections of solar activity generated very little interest from the climate science community, despite the large impact it would have on climate (Archibald, 2006, 2007). The basis of Clilverd’s prediction was a model for sunspot number using low-frequency solar oscillations, with periods of 22, 53, 88, 106, 213, and 420 years modulating the 11-year Schwabe cycle. The model predicts a period of quiet solar activity lasting until approximately 2030 fol- lowed by a recovery during the middle of the century to more typical solar activity cycles with peak sunspot numbers around 120. The graphs in Figs. 1e15 show data related to solar activity. Additional data may be found in Archibald (2010). The Eddy Minimum (Fig. 1) has started 210 years after the start of the Dalton Minimum, consistent with it being a de Vries Cycle event. The graph in Fig. 2 shows that Solar Cycles 3 and 4, leading up to the Dalton Minimum, are very similar in amplitude and morphology to Solar Cycles 22 and 23, leading up to the current minimum. The two data sets are aligned on the month of transition between Solar Cycles 4 and 5 and between Solar Cycles 23 and 24. In the absence of a significant change in Total Solar Irradiance over the solar cycle, modulation of the Earth’s climate by the changing flux in galactic cosmic 200 180 Projected 160 Dalton Eddy Minimum Minimum 140 120 100 80 60 4 5 24 25 40 20 0 1701 1731 1761 1791 1821 1851 1881 1911 1941 1971 2001 2031 FIGURE 1 Solar cycle amplitude 1701e2045. Chapter j 11 The Current Solar Minimum 279 180 Solar Cycle 3 Solar Cycle 23 compared to Solar Cycle 4 160 Aligned on month of minimum Solar Cycle 22 140 Solar Cycle 4 120 100 Solar Cycle 23 80 Dalton Minimum 60 Solar Cycle 5 Solar Cycle 6 Solar Cycle Amplitude 40 May 2010 20 0 1777 1781 1785 1789 1793 1797 1801 1805 1809 1813 1817 FIGURE 2 Similarity between precursor cycles. 1.8 Maunder Sporer Minimum Dalton 1.6 Minimum Minimum Decreasing Galactic 1.4 Cosmic Rays 1.2 1.0 0.8 0.6 Modern Little Ice Age 0.4 Warm Period 0.2 0.0 1425 1485 1545 1605 1665 1725 1785 1845 1905 1965 FIGURE 3 Be10 from the Dye 3 ice core, Greenland Plateau. rays was proposed by Svensmark and Friis-Christensen (1997). The Dye 3 Be10 record (Fig.3) shows a correlation between spikes in Be10 and cold periods for the last 600 years. It also shows a steep decline in Be10 in the Modern Warm Period, suggesting a solar origin for this warming. Usokin et al. (2005) found 280 PART j IV Solar Activity 12 Interplanetary Magnetic Field smoothed 27 day average 10 1970s cooling period 8 6 nanoTeslas 4 2 Solar Cycle 20 Solar Cycle 21 Solar Cycle 22 Solar Cycle 23 0 1966 1970 1973 1977 1980 1984 1987 1991 1994 1998 2001 2005 2009 FIGURE 4 Interplanetary Magnetic Field 1966e2010. 300 250 Solar Cycle 23 1970s Cooling Period 200 Projection 150 Solar Flux Units Flux Solar 100 50 F10.7 Flux 1948 - 2020 0 1948 1953 1958 1963 1968 1973 1978 1983 1988 1993 1998 2003 2008 2013 2018 FIGURE 5 F10.7 flux 1948e2020. that the level of solar activity during the past 70 years is exceptional, and the previous period of equally high activity occurred more than 8,000 years ago. The strength of the Interplanetary Magnetic Field (Fig. 4) has fallen to levels below that of previous solar cycle transitions. What is also interesting in Chapter j 11 The Current Solar Minimum 281 40 aa Index 35 1970s 1868 - 2010 Cooling Period 30 25 20 15 10 Increasing Solar Activity 5 Little Ice Age Modern Warm Period 0 1868 1888 1908 1928 1948 1968 1988 2008 FIGURE 6 The aa Index 1868e2010. 7500 Oulu Neutron Count 23/24 Solar 1964 - 2009 Minimum 21/22 Solar 22/23 Solar 7000 1970s Cooling Minimum Minimum Period 6500 6000 5500 5000 Monthly Average Counts per Minute Data: Sodankyla Geophysical Observatory 4500 1964 1968 1972 1976 1980 1984 1988 1992 1996 2000 2004 2008 FIGURE 7 Oulu, Finland neutron monitor count 1960e2010. this data is the flatness of this solar magnetic indicator during the 1970s cooling period. The F10.7 index (Fig. 5) is a measure of the solar radio flux near the peak of the observed solar radio emission. Emission from the Sun at radio wavelengths 282 PART j IV Solar Activity FIGURE 8 The correlation between solar cycle length and mean annual temperature at Armagh, Northern Ireland. 1.6 1.4 Archangel, Russia rsq = 0.38 1.2 1.0 Correlation = 0.6 degrees/annum 0.8 0.6 0.4 Degrees Celsius 0.2 0.0 -0.2 -0.4 9 9.5 10 10.5 11 11.5 12 12.5 13 Solar Cycle Length Years FIGURE 9 Archangel, Russia e solar cycle length relative to average annual temperature. Chapter j 11 The Current Solar Minimum 283 10.5 Providence, Rhode Island 10.0 rsq = 0.38 9.5 9.0 8.5 Correlation = 0.62 degrees/annum Degrees Celsius 8.0 7.5 7.0 9.0 9.5 10.0 10.5 11.0 11.5 12.0 12.5 13.0 Solar Cycle Length Years FIGURE 10 Providence, Rhode Island e solar cycle length relative to average annual temperature. 8.5 Hanover, New Hampshire 8.0 rsq = 0.53 7.5 7.0 6.5 Correlation = 0.73 degrees/annum Degrees Celsius 6.0 5.5 5.0 9.0 9.5 10.0 10.5 11.0 11.5 12.0 12.5 13.0 Solar Cycle Length Years FIGURE 11 Hanover, New Hampshire e solar cycle length relative to average annual temperature. 284 PART j IV Solar Activity 12.0 11.5 West Chester, Pennsylvania rsq = 0.29 11.0 10.5 10.0 Degree Celsius 9.5 Correlation = 0.5 degrees/annum 9.0 8.5 8.0 9.0 9.5 10.0 10.5 11.0 11.5 12.0 12.5 13.0 Solar Cycle Length Years FIGURE 12 West Chester, Pennsylvania e solar cycle length relative to average annual temperature. 8.5 Portland, Maine 8.0 rsq = 0.49 7.5 7.0 6.5 Degree Celsius 6.0 Correlation = 0.70 degrees/annum 5.5 5.0 9.0 9.5 10.0 10.5 11.0 11.5 12.0 12.5 13.0 Solar Cycle Length Years FIGURE 13 Portland, Maine e solar cycle length relative to average annual temperature. is due primarily to diffuse, non-radiative heating of coronal plasma trapped in the magnetic fields overlying active regions. It is the best indicator of overall solar activity levels and is not subject to observer bias in the way that the counting of sunspots is. The graph above shows the F10.7 flux from 1948 with Chapter j 11 The Current Solar Minimum 285 300 200 17 23 15 21 19 100 0 -100 Solar Cycle Amplitude 20 S.C. 24 S.C. 25 16 22 -200 18 Eddy Minimum -300 1914 1924 1934 1944 1954 1964 1974 1984 1994 2004 2014 2024 2034 2044 FIGURE 14 The ability to look forward using a model of solar activity. 4 Parana River Streamflow 3 2 1 Sunspot Number 0 -1 -2 -3 -4 1909 1919 1929 1939 1949 1959 1969 1979 1989 FIGURE 15 The correlation between the de-trended time series for the Parana River stream flow and sunspot number. a projection to 2020. Note the lower activity of the 1970s cooling period. Activity over the next 10 years is projected to be much lower again.
Recommended publications
  • → Investigating Solar Cycles a Soho Archive & Ulysses Final Archive Tutorial
    → INVESTIGATING SOLAR CYCLES A SOHO ARCHIVE & ULYSSES FINAL ARCHIVE TUTORIAL SCIENCE ARCHIVES AND VO TEAM Tutorial Written By: Madeleine Finlay, as part of an ESAC Trainee Project 2013 (ESA Student Placement) Tutorial Design and Layout: Pedro Osuna & Madeleine Finlay Tutorial Science Support: Deborah Baines Acknowledgements would like to be given to the whole SAT Team for the implementation of the Ulysses and Soho archives http://archives.esac.esa.int We would also like to thank; Benjamín Montesinos, Department of Astrophysics, Centre for Astrobiology (CAB, CSIC-INTA), Madrid, Spain for having reviewed and ratified the scientific concepts in this tutorial. CONTACT [email protected] [email protected] ESAC Science Archives and Virtual Observatory Team European Space Agency European Space Astronomy Centre (ESAC) Tutorial → CONTENTS PART 1 ....................................................................................................3 BACKGROUND ..........................................................................................4-5 THE EXPERIMENT .......................................................................................6 PART 1 | SECTION 1 .................................................................................7-8 PART 1 | SECTION 2 ...............................................................................9-11 PART 2 ..................................................................................................12 BACKGROUND ........................................................................................13-14
    [Show full text]
  • Level and Length of Cyclic Solar Activity During the Maunder Minimum As Deduced from the Active-Day Statistics
    A&A 577, A71 (2015) Astronomy DOI: 10.1051/0004-6361/201525962 & c ESO 2015 Astrophysics Level and length of cyclic solar activity during the Maunder minimum as deduced from the active-day statistics J. M. Vaquero1,G.A.Kovaltsov2,I.G.Usoskin3, V. M. S. Carrasco4, and M. C. Gallego4 1 Departamento de Física, Universidad de Extremadura, 06800 Mérida, Spain 2 Ioffe Physical-Technical Institute, 194021 St. Petersburg, Russia 3 Sodankylä Geophysical Observatory and ReSoLVE Center of Excellence, University of Oulu, 90014 Oulu, Finland e-mail: [email protected] 4 Departamento de Física, Universidad de Extremadura, 06071 Badajoz, Spain Received 25 February 2015 / Accepted 25 March 2015 ABSTRACT Aims. The Maunder minimum (MM) of greatly reduced solar activity took place in 1645–1715, but the exact level of sunspot activity is uncertain because it is based, to a large extent, on historical generic statements of the absence of spots on the Sun. Using a conservative approach, we aim to assess the level and length of solar cycle during the MM on the basis of direct historical records by astronomers of that time. Methods. A database of the active and inactive days (days with and without recorded sunspots on the solar disc) is constructed for three models of different levels of conservatism (loose, optimum, and strict models) regarding generic no-spot records. We used the active day fraction to estimate the group sunspot number during the MM. Results. A clear cyclic variability is found throughout the MM with peaks at around 1655–1657, 1675, 1684, 1705, and possibly 1666, with the active-day fraction not exceeding 0.2, 0.3, or 0.4 during the core MM, for the three models.
    [Show full text]
  • Statistical Properties of Superactive Regions During Solar Cycles 19–23⋆
    A&A 534, A47 (2011) Astronomy DOI: 10.1051/0004-6361/201116790 & c ESO 2011 Astrophysics Statistical properties of superactive regions during solar cycles 19–23 A. Q. Chen1,2,J.X.Wang1,J.W.Li2,J.Feynman3, and J. Zhang1 1 Key Laboratory of Solar Activity of Chinese Academy of Sciences, National Astronomical Observatories, Chinese Academy of Sciences, PR China e-mail: [email protected]; [email protected] 2 National Center for Space Weather, China Meteorological Administration, PR China 3 Helio research, 5212 Maryland Avenue, La Crescenta, USA Received 26 February 2011 / Accepted 20 August 2011 ABSTRACT Context. Each solar activity cycle is characterized by a small number of superactive regions (SARs) that produce the most violent of space weather events with the greatest disastrous influence on our living environment. Aims. We aim to re-parameterize the SARs and study the latitudinal and longitudinal distributions of SARs. Methods. We select 45 SARs in solar cycles 21–23, according to the following four parameters: 1) the maximum area of sunspot group, 2) the soft X-ray flare index, 3) the 10.7 cm radio peak flux, and 4) the variation in the total solar irradiance. Another 120 SARs given by previous studies of solar cycles 19–23 are also included. The latitudinal and longitudinal distributions of the 165 SARs in both the Carrington frame and the dynamic reference frame during solar cycles 19–23 are studied statistically. Results. Our results indicate that these 45 SARs produced 44% of all the X class X-ray flares during solar cycles 21–23, and that all the SARs are likely to produce a very fast CME.
    [Show full text]
  • Properties of the Solar Velocity Field Indicated by Motions of Sunspot Groups and Coronal Bright Points
    DISSERTATION zur Erlangung des Doktorgrades an der Naturwissenschaflichen Fakultät der Karl-Franzens-Universität Graz Properties of the solar velocity field indicated by motions of sunspot groups and coronal bright points Ivana Poljančić Beljan begutachtet von Univ.-Prof. Dr. Arnold Hanslmeier Institut für Physik Karl-Franzens-Universität Graz und Dr. Roman Brajša, scientific advisor Hvar Observatory, Faculty of Geodesy University of Zagreb 2018 Thesis advisor: Univ.-Prof. Dr. Hanslmeier Arnold Ivana Poljančić Beljan Properties of the solar velocity field indicated by motions of sunspot groups and coronal bright points Abstract The solar dynamo is a consequence of the interaction of the solar magnetic field with the large scale plasma motions, namely differential rotation and meridional flows. The main aims of the dissertation are to present precise measurements of the solar differential rotation, to improve insights in the relationship between the solar rotation and activity, to clarify the cause of the existence of a whole range of different results obtained for meridional flows and to clarify that the observed transfer of the angular momentum to- wards the solar equator mainly depends on horizontal Reynolds stress. For each of the mentioned topics positions of sunspot groups and coronal bright points (CBPs) from five different sources have been used. Synodic angular rotation velocities have been calculated using the daily shift or linear least-square fit methods. After the conversion to sidereal values, differential rotation profiles have been calculated by the least-square fitting. Covariance of the calculated rotational and meridional velocities was used to de- rive the horizontal Reynolds stress. The analysis of the differential rotation in general has shown that Kanzelhöhe Observatory for Solar and Environmental research (KSO) provides a valuable data set with a satisfactory accuracy suitable for the investigation of differential rotation and similar studies.
    [Show full text]
  • Prediction of Solar Activity on the Basis of Spectral Characteristics of Sunspot Number
    Annales Geophysicae (2004) 22: 2239–2243 SRef-ID: 1432-0576/ag/2004-22-2239 Annales © European Geosciences Union 2004 Geophysicae Prediction of solar activity on the basis of spectral characteristics of sunspot number E. Echer1, N. R. Rigozo1,2, D. J. R. Nordemann1, and L. E. A. Vieira1 1Instituto Nacional de Pesquisas Espaciais (INPE), Av. Astronautas, 1758 ZIP 12201-970, Sao˜ Jose´ dos Campos, SP, Brazil 2Faculdade de Tecnologia Thereza Porto Marques (FAETEC) ZIP 12308-320, Jacare´ı, Brazil Received: 9 July 2003 – Revised: 6 February 2004 – Accepted: 18 February 2004 – Published: 14 June 2004 Abstract. Prediction of solar activity strength for solar cy- when daily averages are more frequently available (Hoyt and cles 23 and 24 is performed on the basis of extrapolation of Schatten, 1998a, b). sunspot number spectral components. Sunspot number data When the solar cycle is in its maximum phase, there are during 1933–1996 periods (solar cycles 17–22) are searched important terrestrial consequences, such as the higher solar for periodicities by iterative regression. The periods signifi- emission of extreme-ultraviolet and ultraviolet flux, which cant at the 95% confidence level were used in a sum of sine can modulate the middle and upper terrestrial atmosphere, series to reconstruct sunspot series, to predict the strength and total solar irradiance, which could have effects on terres- of solar cycles 23 and 24. The maximum peak of solar cy- trial climate (Hoyt and Schatten, 1997), as well as the coronal cles is adequately predicted (cycle 21: 158±13.2 against an mass ejection and interplanetary shock rates, responsible by observed peak of 155.4; cycle 22: 178±13.2 against 157.6 geomagnetic activity storms and auroras (Webb and Howard, observed).
    [Show full text]
  • Coronal Mass Ejections and Solar Radio Emissions
    CORONAL MASS EJECTIONS AND SOLAR RADIO EMISSIONS N. Gopalswamy∗ Abstract Three types of low-frequency nonthermal radio bursts are associated with coro- nal mass ejections (CMEs): Type III bursts due to accelerated electrons propagating along open magnetic field lines, type II bursts due to electrons accelerated in shocks, and type IV bursts due to electrons trapped in post-eruption arcades behind CMEs. This paper presents a summary of results obtained during solar cycle 23 primarily using the white-light coronagraphic observations from the Solar Heliospheric Ob- servatory (SOHO) and the WAVES experiment on board Wind. 1 Introduction Coronal mass ejections (CMEs) are associated with a whole host of radio bursts caused by nonthermal electrons accelerated during the eruption process. Radio bursts at low frequencies (< 15 MHz) are of particular interest because they are associated with ener- getic CMEs that travel far into the interplanetary (IP) medium and affect Earth’s space environment if Earth-directed. Low frequency radio emission needs to be observed from space because of the ionospheric cutoff (see Fig. 1), although some radio instruments permit observations down to a few MHz [Erickson 1997; Melnik et al., 2008]. Three types of radio bursts are prominent at low frequencies: type III, type II, and type IV bursts, all due to nonthermal electrons accelerated during solar eruptions. The radio emission is thought to be produced by the plasma emission mechanism [Ginzburg and Zheleznyakov, 1958], involving the generation of Langmuir waves by nonthermal electrons accelerated during the eruption and the conversion of Langmuir waves to electromagnetic radiation. Langmuir waves scattered off of ions or low-frequency turbulence result in radiation at the fundamental (or first harmonic) of the local plasma frequency.
    [Show full text]
  • On Polar Magnetic Field Reversal in Solar Cycles 21, 22, 23, and 24
    On Polar Magnetic Field Reversal in Solar Cycles 21, 22, 23, and 24 Mykola I. Pishkalo Main Astronomical Observatory, National Academy of Sciences, 27 Zabolotnogo vul., Kyiv, 03680, Ukraine [email protected] Abstract The Sun’s polar magnetic fields change their polarity near the maximum of sunspot activity. We analyzed the polarity reversal epochs in Solar Cycles 21 to 24. There were a triple reversal in the N-hemisphere in Solar Cycle 24 and single reversals in the rest of cases. Epochs of the polarity reversal from measurements of the Wilcox Solar Observatory (WSO) are compared with ones when the reversals were completed in the N- and S-hemispheres. The reversal times were compared with hemispherical sunspot activity and with the Heliospheric Current Sheet (HCS) tilts, too. It was found that reversals occurred at the epoch of the sunspot activity maximum in Cycles 21 and 23, and after the corresponding maxima in Cycles 22 and 24, and one-two years after maximal HCS tilts calculated in WSO. Reversals in Solar Cycles 21, 22, 23, and 24 were completed first in the N-hemisphere and then in the S-hemisphere after 0.6, 1.1, 0.7, and 0.9 years, respectively. The polarity inversion in the near-polar latitude range ±(55–90)˚ occurred from 0.5 to 2.0 years earlier that the times when the reversals were completed in corresponding hemisphere. Using the maximal smoothed WSO polar field as precursor we estimated that amplitude of Solar Cycle 25 will reach 116±12 in values of smoothed monthly sunspot numbers and will be comparable with the current cycle amplitude equaled to 116.4.
    [Show full text]
  • Galactic Cosmic Ray Radiation Hazard in the Unusual Extended Solar Minimum Between Solar Cycle 23 and 24
    1 Galactic Cosmic Ray Radiation Hazard in the Unusual Extended Solar 2 Minimum between Solar Cycle 23 and 24 3 4 N. A. Schwadron, A. J. Boyd, K. Kozarev 5 Boston University, Boston, Mass, USA 6 M. Golightly, H. Spence 7 University of New Hampshire, Durham New Hampshire, USA 8 L. W. Townsend 9 University of Tennessee, Knoxville, TN, USA 10 M. Owens 11 Space Environment Physics Group, Department of Meteorology, University of Reading, 12 UK 13 14 Abstract. Galactic Cosmic Rays (GCRs) are extremely difficult to shield against and 15 pose one of most severe long-term hazards for human exploration of space. The recent 16 solar minimum between solar cycle 23 and 24 shows a prolonged period of reduced solar 17 activity and low interplanetary magnetic field strengths. As a result, the modulation of 18 GCRs is very weak, and the fluxes of GCRs are near their highest levels in the last 25 19 years in the Fall of 2009. Here, we explore the dose-rates of GCRs in the current 20 prolonged solar minimum and make predictions for the Lunar Reconnaissance Orbiter 21 (LRO) Cosmic Ray Telescope for the Effects of Radiation (CRaTER), which is now 22 measuring GCRs in the lunar environment. Our results confirm the weak modulation of 23 GCRs leading to the largest dose rates seen in the last 25 years over a prolonged period of 24 little solar activity. 25 26 Background – Galactic Cosmic Rays and Human Health 27 28 In balloon flights in 1912-1913, Hess first measured a form of radiation that intensified 29 with altitude [Hess, 1912; 1913].
    [Show full text]
  • Nonaxisymmetric Component of Solar Activity and the Gnevyshev-Ohl Rule
    Solar Physics DOI: 10.1007/•••••-•••-•••-••••-• Nonaxisymmetric Component of Solar Activity and the Gnevyshev-Ohl rule E.S.Vernova1 · M.I. Tyasto1 · D.G. Baranov2 · O.A. Danilova1 c Springer •••• Abstract The vector representation of sunspots is used to study the non- axisymmetric features of the solar activity distribution (sunspot data from Greenwich–USAF/NOAA, 1874–2016).The vector of the longitudinal asym- metry is defined for each Carrington rotation; its modulus characterizes the magnitude of the asymmetry, while its phase points to the active longitude. These characteristics are to a large extent free from the influence of a stochastic component and emphasize the deviations from the axisymmetry. For the sunspot area, the modulus of the vector of the longitudinal asymmetry changes with the 11-year period; however, in contrast to the solar activity, the amplitudes of the asymmetry cycles obey a special scheme. Each pair of cycles from 12 to 23 follows in turn the Gnevyshev–Ohl rule (an even solar cycle is lower than the following odd cycle) or the “anti-Gnevyshev–Ohl rule” (an odd solar cycle is lower than the preceding even cycle). This effect is observed in the longitudinal asymmetry of the whole disk and the southern hemisphere. Possibly, this effect is a manifes- tation of the 44-year structure in the activity of the Sun. Northern hemisphere follows the Gnevyshev–Ohl rule in Solar Cycles 12–17, while in Cycles 18–23 the anti-rule is observed. Phase of the longitudinal asymmetry vector points to the dominating (active) longitude. Distribution of the phase over the longitude was studied for two periods of the solar cycle, ascent-maximum and descent-minimum, separately.
    [Show full text]
  • Variations of the Galactic Cosmic Rays in the Recent Solar Cycles
    Draft version April 19, 2021 Typeset using LATEX manuscript style in AASTeX63 Variations of the Galactic Cosmic Rays in the Recent Solar Cycles Shuai Fu ,1, 2 Xiaoping Zhang ,1, 2 Lingling Zhao ,3 and Yong Li 1, 2 1State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology, Taipa 999078, Macau, PR China 2CNSA Macau Center for Space Exploration and Science, Taipa 999078, Macau, PR China 3Center for Space Plasma and Aeronomic Research (CSPAR), University of Alabama in Huntsville, Huntsville, AL 35805, USA Submitted to ApJS ABSTRACT In this paper, we study the galactic cosmic ray (GCR) variations over the solar cy- cles 23 and 24, with measurements from the NASA's ACE/CRIS instrument and the ground-based neutron monitors (NMs). The results show that the maximum GCR intensities of heavy nuclei (5 6 Z 6 28, 50∼500 MeV/nuc) at 1 AU during the so- lar minimum in 2019{2020 break their previous records, exceeding those recorded in 1997 and 2009 by ∼25% and ∼6%, respectively, and are at the highest levels since the space age. However, the peak NM count rates are lower than those in late 2009. The arXiv:2104.07862v1 [astro-ph.SR] 16 Apr 2021 difference between GCR intensities and NM count rates still remains to be explained. Furthermore, we find that the GCR modulation environment during the solar minimum P24=25 are significantly different from previous solar minima in several aspects, including Corresponding author: Xiaoping Zhang [email protected] Corresponding author: Lingling Zhao [email protected] 2 Fu et al.
    [Show full text]
  • ESA Bulletin No
    MARSDEN 6/12/03 5:08 PM Page 60 Artist’s impression of Ulysses’ exploratory mission (by D. Hardy) Science 60 esa bulletin 114 - may 2003 www.esa.int MARSDEN 6/12/03 5:08 PM Page 61 News from the Sun’s Poles News from the Sun’s Poles Courtesy of Ulysses Richard G. Marsden ESA Directorate of Scientific Programmes, ESTEC, Noordwijk, The Netherlands Edward J. Smith Jet Propulsion Laboratory, California Institute of Technology, Pasadena, USA True to its classical namesake in Dante’s Introduction Launched from Cape Canaveral more than 13 years ago, Ulysses Inferno, the ESA-NASA Ulysses mission has is well on its way to completing two full circuits of the Sun in a unique orbit that takes it over the north and south poles of our ventured into the ‘unpeopled world star. In doing so, the European-built space probe and its payload of scientific instruments have added a fundamentally new beyond the Sun’,in the pursuit of perspective to our knowledge of the bubble in space in which the Sun and the Solar System exist, called ‘the heliosphere’. ‘knowledge high’! www.esa.int esa bulletin 114 - may 2003 61 MARSDEN 6/12/03 5:09 PM Page 62 Science A small spacecraft by today’s standards, Ulysses weighed just 367 kg at launch, including its scientific payload of 55 kg. The nine scientific instruments on board measure the solar wind, the heliospheric magnetic field, natural radio emission and plasma waves, energetic particles and cosmic rays, interplanetary and interstellar dust, neutral interstellar helium atoms, and cosmic gamma-ray bursts.
    [Show full text]
  • Pecularities of Cosmic Ray Modulation in the Solar Minimum 23/24
    PECULARITIES OF COSMIC RAY MODULATION IN THE SOLAR MINIMUM 23/24. M. V. Alania 1,2, R. Modzelewska 1 and A. Wawrzynczak 3 1 Institute Math. & Physics, Siedlce University, 3 Maja 54, 08-110 Siedlce, Poland. 2 Institute of Geophysics, Tbilisi State University, Tbilisi, Georgia. 3Institute of Computer Science, Siedlce University, 3 Maja 54, 08-110 Siedlce, Poland. [email protected], [email protected], [email protected], Abstract We study changes of the galactic cosmic ray (GCR) intensity for the ending period of the solar cycle 23 and the beginning of the solar cycle 24 using neutron monitors experimental data. We show that an increase of the GCR intensity in 2009 is generally related with decrease of the solar wind velocity U, the strength B of the interplanetary magnetic field (IMF), and the drift in negative (A<0) polarity epoch. We present that temporal changes of rigidity dependence of the GCR intensity variation before reaching maximum level in 2009 and after it, do not noticeably differ from each other. The rigidity spectrum of the GCR intensity variations calculated based on neutron monitors data (for rigidities > 10 GV) is hard in the minimum and near minimum epoch. We do not recognize any non-ordinary changes in the physical mechanism of modulation of the GCR intensity in the rigidity range of GCR particles to which neutron monitors respond. We compose 2-D non stationary model of transport equation to describe variations of the GCR intensity for 1996-2012 including the A>0 (1996-2001) and the A<0 (2002-2012) periods; diffusion coefficient of cosmic rays for rigidity 10-15 GV is increased by ~ 30% in 2009 (A<0) comparing with 1996 (A>0).
    [Show full text]