Total Solar Irradiance Variability and the Solar Activity Cycle
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→ 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 -
A Spectral Solar/Climatic Model H
A Spectral Solar/Climatic Model H. PRESCOTT SLEEPER, JR. Northrop Services, Inc. The problem of solar/climatic relationships has prove our understanding of solar activity varia- been the subject of speculation and research by a tions have been based upon planetary tidal forces few scientists for many years. Understanding the on the Sun (Bigg, 1967; Wood and Wood, 1965.) behavior of natural fluctuations in the climate is or the effect of planetary dynamics on the motion especially important currently, because of the pos- of the Sun (Jose, 1965; Sleeper, 1972). Figure 1 sibility of man-induced climate changes ("Study presents the sunspot number time series from of Critical Environmental Problems," 1970; "Study 1700 to 1970. The mean 11.1-yr sunspot cycle is of Man's Impact on Climate," 1971). This paper well known, and the 22-yr Hale magnetic cycle is consists of a summary of pertinent research on specified by the positive and negative designation. solar activity variations and climate variations, The magnetic polarity of the sunspots has been together with the presentation of an empirical observed since 1908. The cycle polarities assigned solar/climatic model that attempts to clarify the prior to that date are inferred from the planetary nature of the relationships. dynamic effects studied by Jose (1965). The sun- The study of solar/climatic relationships has spot time series has certain important characteris- been difficult to develop because of an inadequate tics that will be summarized. understanding of the detailed mechanisms respon- sible for the interaction. The possible variation of Secular Cycles stratospheric ozone with solar activity has been The sunspot cycle magnitude appears to in- discussed by Willett (1965) and Angell and Kor- crease slowly and fall rapidly with an. -
Predicting Maximum Sunspot Number in Solar Cycle 24 Nipa J Bhatt
J. Astrophys. Astr. (2009) 30, 71–77 Predicting Maximum Sunspot Number in Solar Cycle 24 Nipa J Bhatt1,∗, Rajmal Jain2 & Malini Aggarwal2 1C. U. Shah Science College, Ashram Road, Ahmedabad 380 014, India. 2Physical Research Laboratory, Navrangpura, Ahmedabad 380 009, India. ∗e-mail: [email protected] Received 2008 November 22; accepted 2008 December 23 Abstract. A few prediction methods have been developed based on the precursor technique which is found to be successful for forecasting the solar activity. Considering the geomagnetic activity aa indices during the descending phase of the preceding solar cycle as the precursor, we predict the maximum amplitude of annual mean sunspot number in cycle 24 to be 111 ± 21. This suggests that the maximum amplitude of the upcoming cycle 24 will be less than cycles 21–22. Further, we have estimated the annual mean geomagnetic activity aa index for the solar maximum year in cycle 24 to be 20.6 ± 4.7 and the average of the annual mean sunspot num- ber during the descending phase of cycle 24 is estimated to be 48 ± 16.8. Key words. Sunspot number—precursor prediction technique—geo- magnetic activity index aa. 1. Introduction Predictions of solar and geomagnetic activities are important for various purposes, including the operation of low-earth orbiting satellites, operation of power grids on Earth, and satellite communication systems. Various techniques, namely, even/odd behaviour, precursor, spectral, climatology, recent climatology, neural networks have been used in the past for the prediction of solar activity. Many investigators (Ohl 1966; Kane 1978, 2007; Thompson 1993; Jain 1997; Hathaway & Wilson 2006) have used the ‘precursor’ technique to forecast the solar activity. -
Solar Wind Variation with the Cycle I. S. Veselovsky,* A. V. Dmitriev
J. Astrophys. Astr. (2000) 21, 423–429 Solar Wind Variation with the Cycle I. S. Veselovsky,* A. V. Dmitriev, A. V. Suvorova & M. V. Tarsina, Institute of Nuclear Physics, Moscow State University, 119899 Moscow, Russia. *e-mail: [email protected] Abstract. The cyclic evolution of the heliospheric plasma parameters is related to the time-dependent boundary conditions in the solar corona. “Minimal” coronal configurations correspond to the regular appearance of the tenuous, but hot and fast plasma streams from the large polar coronal holes. The denser, but cooler and slower solar wind is adjacent to coronal streamers. Irregular dynamic manifestations are present in the corona and the solar wind everywhere and always. They follow the solar activity cycle rather well. Because of this, the direct and indirect solar wind measurements demonstrate clear variations in space and time according to the minimal, intermediate and maximal conditions of the cycles. The average solar wind density, velocity and temperature measured at the Earth's orbit show specific decadal variations and trends, which are of the order of the first tens per cent during the last three solar cycles. Statistical, spectral and correlation characteristics of the solar wind are reviewed with the emphasis on the cycles. Key words. Solar wind—solar activity cycle. 1. Introduction The knowledge of the solar cycle variations in the heliospheric plasma and magnetic fields was initially based on the indirect indications gained from the observations of the Sun, comets, cosmic rays, geomagnetic perturbations, interplanetary scintillations and some other ground-based methods. Numerous direct and remote-sensing space- craft measurements in situ have continuously broadened this knowledge during the past 40 years, which can be seen from the original and review papers. -
Solar Orbiter and Sentinels
HELEX: Heliophysical Explorers: Solar Orbiter and Sentinels Report of the Joint Science and Technology Definition Team (JSTDT) PRE-PUBLICATION VERSION 1 Contents HELEX Joint Science and Technology Definition Team .................................................................. 3 Executive Summary ................................................................................................................................. 4 1.0 Introduction ........................................................................................................................................ 6 1.1 Heliophysical Explorers (HELEX): Solar Orbiter and the Inner Heliospheric Sentinels ........ 7 2.0 Science Objectives .............................................................................................................................. 8 2.1 What are the origins of the solar wind streams and the heliospheric magnetic field? ............. 9 2.2 What are the sources, acceleration mechanisms, and transport processes of solar energetic particles? ........................................................................................................................................ 13 2.3 How do coronal mass ejections evolve in the inner heliosphere? ............................................. 16 2.4 High-latitude-phase science ......................................................................................................... 19 3.0 Measurement Requirements and Science Implementation ........................................................ 20 -
Lectures 6, 7 and 8 October 8, 10 and 13 the Heliosphere
ESSESS 77 LecturesLectures 6,6, 77 andand 88 OctoberOctober 8,8, 1010 andand 1313 TheThe HeliosphereHeliosphere The Exploding Sun • We have seen that at times the Sun explosively sends plasma into the surrounding space. • This occurs most dramatically during CMEs. The History of the Solar Wind • 1878 Becquerel (won Noble prize for his discovery of radioactivity) suggests particles from the Sun were responsible for aurora • 1892 Fitzgerald (famous Irish Mathematician) suggests corpuscular radiation (from flares) is responsible for magnetic storms The Sun’s Atmosphere Extends far into Space 2008 Image 1919 Negative The Sun’s Atmosphere Extends Far into Space • The image of the solar corona in the last slide was taken with a natural occulting disk – the moon’s shadow. • The moon’s shadow subtends the surface of the Sun. • That the Sun had a atmosphere that extends far into space has been know for centuries- we are actually seeing sunlight scattered off of electrons. A Solar Wind not a Stationary Atmosphere • The Earth’s atmosphere is stationary. The Sun’s atmosphere is not stable but is blown out into space as the solar wind filling the solar system and then some. • The first direct measurements of the solar wind were in the 1960’s but it had already been suggested in the early 1900s. – To explain a correlation between auroras and sunspots Birkeland [1908] suggested continuous particle emission from these spots. – Others suggested that particles were emitted from the Sun only during flares and that otherwise space was empty [Chapman and Ferraro, 1931]. Discovery of the Solar Wind • That it is continuously expelled as a wind (the solar wind) was realized when Biermann [1951] noticed that comet tails pointed away from the Sun even when the comet was moving away from the Sun. -
Can You Spot the Sunspots?
Spot the Sunspots Can you spot the sunspots? Description Use binoculars or a telescope to identify and track sunspots. You’ll need a bright sunny day. Age Level: 10 and up Materials • two sheets of bright • Do not use binoculars whose white paper larger, objective lenses are 50 • a book mm or wider in diameter. • tape • Binoculars are usually described • binoculars or a telescope by numbers like 7 x 35; the larger • tripod number is the diameter in mm of • pencil the objective lenses. • piece of cardboard, • Some binoculars cannot be easily roughly 30 cm x 30 cm attached to a tripod. • scissors • You might need to use rubber • thick piece of paper, roughly bands or tape to safely hold the 10 cm x 10 cm (optional) binoculars on the tripod. • rubber bands (optional) Time Safety Preparation: 5 minutes Do not look directly at the sun with your eyes, Activity: 15 minutes through binoculars, or through a telescope! Do not Cleanup: 5 minutes leave binoculars or a telescope unattended, since the optics can be damaged by too much Sun exposure. 1 If you’re using binoculars, cover one of the objective (larger) lenses with either a lens cap or thick piece of folded paper (use tape, attached to the body of the binoculars, to hold the paper in position). If using a telescope, cover the finderscope the same way. This ensures that only a single image of the Sun is created. Next, tape one piece of paper to a book to make a stiff writing surface. If using binoculars, trace both of the larger, objective lenses in the middle of the piece of cardboard. -
The 2015 Senior Review of the Heliophysics Operating Missions
The 2015 Senior Review of the Heliophysics Operating Missions June 11, 2015 Submitted to: Steven Clarke, Director Heliophysics Division, Science Mission Directorate Jeffrey Hayes, Program Executive for Missions Operations and Data Analysis Submitted by the 2015 Heliophysics Senior Review panel: Arthur Poland (Chair), Luca Bertello, Paul Evenson, Silvano Fineschi, Maura Hagan, Charles Holmes, Randy Jokipii, Farzad Kamalabadi, KD Leka, Ian Mann, Robert McCoy, Merav Opher, Christopher Owen, Alexei Pevtsov, Markus Rapp, Phil Richards, Rodney Viereck, Nicole Vilmer. i Executive Summary The 2015 Heliophysics Senior Review panel undertook a review of 15 missions currently in operation in April 2015. The panel found that all the missions continue to produce science that is highly valuable to the scientific community and that they are an excellent investment by the public that funds them. At the top level, the panel finds: • NASA’s Heliophysics Division has an excellent fleet of spacecraft to study the Sun, heliosphere, geospace, and the interaction between the solar system and interstellar space as a connected system. The extended missions collectively contribute to all three of the overarching objectives of the Heliophysics Division. o Understand the changing flow of energy and matter throughout the Sun, Heliosphere, and Planetary Environments. o Explore the fundamental physical processes of space plasma systems. o Define the origins and societal impacts of variability in the Earth/Sun System. • All the missions reviewed here are needed in order to study this connected system. • Progress in the collection of high quality data and in the application of these data to computer models to better understand the physics has been exceptional. -
Our Sun Has Spots.Pdf
THE A T M O S P H E R I C R E S E R V O I R Examining the Atmosphere and Atmospheric Resource Management Our Sun Has Spots By Mark D. Schneider Aurora Borealis light shows. If you minima and decreased activity haven’t seen the northern lights for called The Maunder Minimum. Is there actually weather above a while, you’re not alone. The end This period coincides with the our earth’s troposphere that con- of Solar Cycle 23 and a minimum “Little Ice Age” and may be an cerns us? Yes. In fact, the US of sunspot activity likely took place indication that it’s possible to fore- Department of Commerce late last year. Now that a new 11- cast long-term temperature trends National Oceanic and over several decades or Atmospheric Administra- centuries by looking at the tion (NOAA) has a separate sun’s irradiance patterns. division called the Space Weather Prediction Center You may have heard (SWPC) that monitors the about 22-year climate weather in space. Space cycles (two 11-year sun- weather focuses on our sun spot cycles) in which wet and its’ cycles of solar activ- periods and droughts were ity. Back in April of 2007, experienced in the Mid- the SWPC made a predic- western U.S. The years tion that the next active 1918, 1936, and 1955 were sunspot or solar cycle would periods of maximum solar begin in March of this year. forcing, but minimum Their prediction was on the precipitation over parts of mark, Solar Cycle 24 began NASA TRACE PROJECT, OF COURTESY PHOTO the U.S. -
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. -
The Flaring and Quiescent Components of the Solar Corona
A&A 488, 1069–1077 (2008) Astronomy DOI: 10.1051/0004-6361:200809355 & c ESO 2008 Astrophysics The flaring and quiescent components of the solar corona C. Argiroffi1,2, G. Peres1,2, S. Orlando2, and F. Reale1,2 1 Dipartimento di Scienze Fisiche ed Astronomiche, Sezione di Astronomia, Università di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy e-mail: [argi;peres;reale]@astropa.unipa.it 2 INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy e-mail: [email protected] Received 5 January 2008 / Accepted 30 April 2008 ABSTRACT Context. The solar corona is a template to understand stellar activity. The Sun is a moderately active star, and its corona differs from that of active stars: for instance, active stellar coronae have a double-peaked emission measure distribution EM(T) with a hot peak at 8−20 MK, while the non-flaring solar corona has one peak at 1−2 MK and, typically, much cooler plasma. Aims. We study the average contribution of flares to the solar emission measure distribution to investigate indirectly the hypothesis that the hot peak in the EM(T) of active stellar coronae is due to a large number of unresolved solar-like flares, and to infer properties about the flare distribution from nano- to macro-flares. Methods. We measure the disk-integrated time-averaged emission measure, EMF(T), of an unbiased sample of solar flares, analyzing uninterrupted GOES/XRS light curves over time intervals of one month. We obtain the EMQ(T) of quiescent corona for the same time intervals from Yohkoh/SXT data. -
Solar Radiation
SOLAR CELLS Chapter 2. Solar Radiation Chapter 2. SOLAR RADIATION 2.1 Solar radiation One of the basic processes behind the photovoltaic effect, on which the operation of solar cells is based, is generation of the electron-hole pairs due to absorption of visible or other electromagnetic radiation by a semiconductor material. Today we accept that electromagnetic radiation can be described in terms of waves, which are characterized by wavelength ( λ ) and frequency (ν ), or in terms of discrete particles, photons, which are characterized by energy ( hν ) expressed in electron volts. The following formulas show the relations between these quantities: ν = c λ (2.1) 1 hc hν = (2.2) q λ In Eqs. 2.1 and 2.2 c is the speed of light in vacuum (2.998 × 108 m/s), h is Planck’s constant (6.625 × 10-34 Js), and q is the elementary charge (1.602 × 10-19 C). For example, a green light can be characterized by having a wavelength of 0.55 × 10-6 m, frequency of 5.45 × 1014 s-1 and energy of 2.25 eV. - 2.1 - SOLAR CELLS Chapter 2. Solar Radiation Only photons of appropriate energy can be absorbed and generate the electron-hole pairs in the semiconductor material. Therefore, it is important to know the spectral distribution of the solar radiation, i.e. the number of photons of a particular energy as a function of wavelength. Two quantities are used to describe the solar radiation spectrum, namely the spectral power density, P(λ), and the photon flux density, Φ(λ) .