April 26


How do Solar Cycles Directly Impact Solar Radiation?

By hacheng1@gmail.com

April 26, 2023

In this comprehensive article, readers will learn about solar cycles and their various characteristics, including formation and mechanics, the 11-year solar cycle, and other solar cycles. The article delves into the characteristics of solar radiation, such as visible light, ultraviolet light, and infrared radiation. It explores the different phases of the solar cycle, like solar minimum and maximum, and their effects on solar radiation.

The article also discusses solar activity features such as sunspots, solar flares, and coronal mass ejections, including their influence on solar radiation. Furthermore, the article covers how solar radiation variations impact Earth’s climate, geomagnetic storms, satellite communications, and biological effects. Finally, it details methods for monitoring and predicting solar cycles, including techniques and tools for observation, modeling, and forecasting, as well as current and future research.

Understanding Solar Cycles

Definition and Overview

A solar cycle is a periodic change in the Sun’s activity, which is determined by the fluctuation in the number of sunspots, solar flares, and other phenomena. These cycles affect various aspects of the Earth’s environment, including its climate, satellite communications, and power distribution systems.

Solar cycles have been observed since ancient times; however, it wasn’t until the early 19th century that the first significant solar cycle was discovered by astronomer Samuel Heinrich Schwabe. Today, understanding solar cycles is essential for predicting solar events, protecting sensitive infrastructure, and preparing for potential space weather events that can impact our daily lives.

Formation and Mechanics

Solar cycles are driven by the Sun’s magnetic activity. The Sun is comprised of a gaseous plasma that conducts electricity, generating magnetic fields. The magnetic fields are driven by a dynamo process that involves the interaction between convection, rotation, and the magnetic fields themselves. The solar dynamo mechanism works with the differential rotation of the Sun’s interior, which means that the equator rotates faster than the poles.

Due to differential rotation and turbulent motions in the convective zone, the Sun’s magnetic field lines become twisted and tangled. This process eventually leads to the emergence of magnetic field lines at the solar surface, leading to the formation of sunspots, which are areas of intense magnetic activity. Regions where these magnetic fields concentrate become cooler and darker, resulting in a lower overall solar output.

11-year Solar Cycle

The most well-known solar cycle is the 11-year solar cycle, also known as the Schwabe cycle. It is characterized by periodicity in sunspot counts and solar activity levels. This cycle consists of alternating periods of increasing and decreasing solar activity, with the number of sunspots peaking roughly every 11 years.

During solar minimum, the Sun exhibits few sunspots and solar activity is at its lowest. In contrast, during solar maximum, the number of sunspots and solar activity is at its highest. This cycle is crucial for understanding the dynamics of the Sun’s magnetic field and has significant implications for Earth’s climate and space weather events. Scientists continue to study this cycle to improve their understanding of solar dynamics and to better predict solar events that may impact Earth.

Other Solar Cycles

In addition to the 11-year solar cycle, there are several other solar cycles that have been observed. Some of these cycles have longer periods, while others have shorter periods. Some of the more widely recognized solar cycles include:

  1. The Hale Cycle (also known as the 22-year magnetic cycle): This cycle involves the polarity of the Sun’s magnetic field, which alternates between the northern and southern hemispheres every approximately 11 years, completing a full reversal back to the original polarity after around 22 years.
  2. The Gleissberg Cycle: This is a longer cycle with a period of about 87-105 years. This cycle is associated with variations in solar irradiance, which is the total amount of solar energy reaching Earth. The Gleissberg Cycle, named after the German meteorologist Julius Gleissberg, is believed to influence Earth’s climate, resulting in alternating warm and cool periods.
  3. The Suess Cycle: With a period of around 200-400 years, this cycle is named after Austrian scientist Hans Suess. This cycle has been linked to variations in radiocarbon concentrations in tree rings, which in turn affect the global temperature.

Understanding these cycles is essential for both scientists and policymakers. They provide valuable information about the underlying mechanisms governing solar activity, enabling more accurate forecasting of space weather events. This knowledge is crucial for developing strategies to safeguard against potential hazards caused by solar events, such as disruptions to power grids, satellite communications, and other critical infrastructure.

Characteristics of Solar Radiation

Solar radiation, popularly known as sunlight, consists of several forms of energy emitted by the sun. These different forms of energy are crucial to understand various phenomena on Earth, including climate change, photosynthesis, and renewable energy generation. The essential characteristics of solar radiation are visible light, ultraviolet light, infrared radiation, and total solar irradiance (TSI).

Visible Light

Visible light, also known as the visible spectrum, constitutes the portion of solar radiation that humans can observe using their eyes. This light occupies a narrow spectrum ranging from approximately 380 to 750 nanometres (nm) in wavelength. Visible light accounts for roughly 43% of the total solar radiation reaching Earth’s surface. When sunlight interacts with Earth’s atmosphere, certain wavelengths are scattered or absorbed, resulting in the sky appearing blue during the day and red or orange during sunrise and sunset.

Visible light is a crucial element in the photosynthesis process for plants. Through photosynthesis, plants convert sunlight into chemical energy that allows them to grow and reproduce. This process also releases oxygen into the atmosphere, supporting the respiration of living organisms, including humans.

In terms of renewable energy, visible light plays a vital role in solar power generation through photovoltaic (PV) technology. PV panels contain semiconductor materials that convert sunlight into electricity by utilizing the energy of photons in the visible light spectrum.

Ultraviolet Light

Ultraviolet (UV) light is a type of electromagnetic radiation with wavelengths shorter than visible light but longer than X-rays, ranging from approximately 10 to 400 nm. Although UV light makes up only a small portion of solar radiation—about 10%—it carries significant energy and can cause damage to living organisms.

UV light is divided into three categories: UVA (320 to 400 nm), UVB (280 to 320 nm), and UVC (100 to 280 nm). UVC radiation is the most dangerous type; however, almost all of it is absorbed by Earth’s atmosphere, primarily by the ozone layer. UVA and UVB radiation can penetrate the atmosphere, with UVB being partially absorbed by the ozone layer.

Exposure to UV radiation is beneficial in small amounts, as it stimulates vitamin D production in the human body. However, prolonged exposure to UV light can lead to various health concerns, such as skin cancer, eye damage, and suppression of the immune system.

Infrared Radiation

Infrared (IR) radiation lies just beyond the visible light spectrum, with wavelengths ranging from approximately 750 nm to 1 millimeter (mm). Infrared radiation accounts for nearly 47% of the total solar radiation reaching Earth’s surface. This portion of solar radiation plays a significant role in heating the Earth’s surface and the lower atmosphere.

Infrared radiation is essential for maintaining the Earth’s energy balance as it serves as the primary mechanism of heat transfer between the atmosphere and surface. As sunlight is absorbed by the Earth’s surface, it is transformed into heat, leading to the emission of infrared radiation. Some of this radiation escapes to space, while part of it is absorbed and re-emitted by greenhouse gases in the atmosphere, creating the greenhouse effect.

In the realm of renewable energy, infrared radiation is also utilized in solar thermal technology for heating water and generating steam to produce electricity in solar power plants.

Total Solar Irradiance (TSI)

Total solar irradiance (TSI) represents the total amount of energy emitted by the sun across all wavelengths of the electromagnetic spectrum, including visible light, ultraviolet light, and infrared radiation. TSI is measured in watts per square meter (W/m²) and is crucial in understanding the Earth’s energy balance and climate change.

TSI values can vary due to fluctuations in solar activity, such as sunspots and solar flares. These variations can influence the Earth’s climate, resulting in changes in temperature, atmospheric circulation, and precipitation patterns.

By understanding the characteristics of solar radiation, scientists and engineers can develop solutions to mitigate climate change, enhance renewable energy technologies, and protect living organisms from harmful radiation effects.

Phases of the Solar Cycle

The solar cycle, also known as the sunspot cycle, is the periodic change in the Sun’s activity and appearance over an approximately 11-year timeframe. It comprises various phases, including the solar minimum and solar maximum, which are associated with different levels of solar activity. These fluctuations in solar phenomena have significant effects on our planet, particularly in terms of solar radiation and the auroras seen near the Earth’s poles.

Solar Minimum

The solar minimum is the phase in the solar cycle where the sun’s activity is relatively low. During this period, the number of sunspots and solar flares decreases, leading to a reduced release of energy and magnetic fields from the solar surface. As a result, the Sun emits less extreme ultraviolet (UV) light, which in turn causes a reduction in the heating and expansion of the Earth’s upper atmosphere.

One significant effect of the solar minimum on Earth is a decrease in geomagnetic storms, which occur when an eruption from the sun’s surface – such as a solar flare or coronal mass ejection (CME) – interacts with Earth’s magnetic field. These storms can cause disruptions in telecommunication and satellite systems, damage electrical power grids, and even endanger astronauts in space.

Another consequence of the solar minimum phase is the increased penetration of galactic cosmic rays into the solar system. During this period, the sun’s magnetic field weakens, enabling high-energy particles from space to enter the inner solar system more easily, which can lead to increased radiation exposure for spacecraft and astronauts.

Finally, during solar minimum, the chances of observing auroras at high latitudes are typically lower. This is because fewer geomagnetic storms caused by solar activity translate to less frequent and less intense auroral activity at the Earth’s poles.

Solar Maximum

The solar maximum, as opposed to the solar minimum, is the phase in which the Sun’s activity reaches its peak. Sunspots, solar flares, and CMEs become more frequent and more intense, leading to a higher release of energy and magnetic fields from the solar surface. Consequently, the Sun emits more extreme UV light, which results in increased heating and expansion of Earth’s upper atmosphere.

One major effect of the solar maximum is a boost in the intensity and frequency of geomagnetic storms. These storms can produce vivid auroras at high latitudes, making them a thrilling sight for skywatchers. However, they also pose potential hazards to technology and infrastructure, as mentioned earlier.

Another effect of the solar maximum is the so-called “solar energetic particle (SEP) events,” which involve the acceleration of charged particles to very high energies. SEPs can be harmful to both spacecraft electronics and astronauts outside the Earth’s protective magnetosphere.

However, increased solar activity during the solar maximum may provide a protective shield against galactic cosmic rays. This is because the sun’s stronger magnetic field tends to deflect high-energy particles from the inner solar system.

Effects on Solar Radiation

The solar cycle’s phases, particularly the solar minimum and solar maximum, have pronounced effects on the amount of solar radiation received by Earth. During the solar maximum, there is an increase in solar radiation due to the increased number and intensity of sunspots, solar flares, and CMEs. This increase in solar radiation leads to a warming of Earth’s upper atmosphere, which can cause a slight fluctuation in global temperatures.

Conversely, when solar activity is at its lowest point during the solar minimum, less solar radiation reaches the Earth. This reduction in solar radiation can lead to a very slight cooling effect on global temperatures. However, these temperature fluctuations induced by the solar cycle are generally small compared to other factors, such as the impact of greenhouse gas emissions on climate change.

In addition to its impact on temperature, changes in solar radiation can influence Earth’s protective ozone layer, primarily in the stratosphere. Enhanced UV radiation during the solar maximum can lead to the increased production and destruction of stratospheric ozone, while reduced UV radiation during the solar minimum has the opposite effect.

In summary, the solar cycle, with its varying phases of solar minimum and solar maximum, has substantial effects on both the Sun’s behavior and our planet. These effects range from auroral displays and solar radiation fluctuations to geomagnetic storms and space weather hazards for electronics and astronauts. Understanding and monitoring the solar cycle is crucial for mitigating potential risks and adapting to the ever-changing conditions in our solar system.

Solar Activity Features and Solar Radiation


Sunspots are dark, temporary regions on the Solar surface, which are cooler and have lower magnetic field strength compared to their surroundings. These features are essential in understanding solar activity and its influence on solar radiation.

Formation and Properties

Sunspots form as a result of the Sun’s magnetic fields, which originate in the Solar interior. When these magnetic fields rise to the surface, they create areas with high magnetic intensity. These areas restrict the transportation of energy from the interior to the surface through convective processes. As a result, the temperature of sunspots is lower, making them cooler and darker compared to the surrounding photosphere.

Sunspots are characterized by two regions: the dark inner core (umbra) and the lighter outer region (penumbra). The umbra has a relatively homogeneous magnetic field, while the penumbra exhibits a more complex field structure. Sunspots have a lifetime ranging from several hours to several months, and their size can vary from small spots to massive groups that span thousands of kilometers.

Influence on Solar Radiation

Sunspots have a direct impact on the Sun’s energy output or total solar irradiance (TSI), which is the primary source of energy for the Earth’s atmosphere and climate. Although sunspots appear darker and cooler than the surrounding photosphere, they are accompanied by active regions that produce more light and energy than an average solar surface area. These active regions around sunspots emit ultraviolet (UV) and X-ray radiation, increasing the Sun’s overall radiation output.

The number of sunspots increases and decreases in an 11-year cycle, referred to as the solar cycle. During times of high sunspot activity, known as solar maximum, the solar radiation output is higher, causing variations in the Earth’s climate, satellites, and communication systems. Conversely, during low sunspot activity, known as solar minimum, the radiation output decreases.

Solar Flares

Solar flares are sudden, intense bursts of electromagnetic radiation that occur in the solar atmosphere, often in connection with sunspots, and significantly influence solar radiation.

Formation and Properties

Solar flares form due to the rapid release of magnetic energy stored in the solar corona. They occur when magnetic fields in the corona become twisted and distorted, leading to a sudden release of energy in the form of light, heat, and accelerated particles. Solar flares are classified based on their X-ray brightness, with the classes being A, B, C, M, and X, in increasing order of intensity.

Solar flares can release a huge amount of energy, equivalent to millions of 100-megaton hydrogen bombs exploding simultaneously. They usually last for a few minutes to several hours and release radiation across the entire electromagnetic spectrum, from radio waves to gamma rays.

Influence on Solar Radiation

Solar flares directly affect the Earth’s atmosphere by increasing the flux of solar radiation, particularly in the X-ray and ultraviolet wavelengths. This increase in radiation can cause the Earth’s atmosphere to heat up and expand, causing communication and navigation satellite disruptions and potential damage.

Solar flares can also cause geomagnetic storms when the emitted solar particles reach Earth and interact with its magnetic field. These geomagnetic storms can lead to auroras, as well as disruptions in power grids, radio communications, and satellite operations.

Coronal Mass Ejections

Coronal mass ejections (CMEs) are significant solar events that release massive amounts of solar plasma and magnetic fields from the Sun’s corona into interplanetary space, directly influencing solar radiation.

Formation and Properties

CMEs occur when magnetic field structures with stored energy in the solar corona become unstable and suddenly release their energy. This process propels a large amount of solar plasma and magnetic fields into space at high speeds. CMEs can occur independently or in association with other solar phenomena, such as solar flares and prominence eruptions.

CMEs vary in size and speed, with some reaching speeds of several million miles per hour. Their frequency also varies throughout the solar cycle, with more CMEs occurring during solar maximum and fewer during solar minimum.

Influence on Solar Radiation

CMEs can significantly impact solar radiation, particularly when they are directed toward Earth. When a CME reaches Earth, it can cause a sudden increase in solar wind pressure, compressing Earth’s magnetic field and inducing a geomagnetic storm.

These storms can result in a range of impacts, including disruptions to power systems, satellite operations, and radio communications. They can also cause damage to orbiting satellites and may even pose a radiation risk to astronauts on space missions.

In summary, solar activity features such as sunspots, solar flares, and coronal mass ejections play a crucial role in shaping solar radiation. Their varying frequencies and intensities directly influence the Earth’s atmosphere and climate, as well as the operation of satellites, power systems, and other technologies.

Effects of Solar Radiation Variations on Earth

Solar radiation is energy emitted by the sun in the form of electromagnetic waves, which include ultraviolet (UV) light, visible light, and infrared (IR) light. The sun’s energy output is not constant but varies over time, influenced by factors such as sunspot activity, solar flares, and coronal mass ejections (CMEs). Variations in solar radiation have both direct and indirect effects on Earth that can impact climate, create geomagnetic storms, affect satellite communications, and cause biological effects related to UV radiation. In this section, we will discuss each of these consequences and their potential implications for our planet and its inhabitants.

Impact on Climate

The Earth’s climate is driven by the balance between incoming solar radiation and outgoing heat (infrared radiation) emitted by the planet. When the sun’s output changes, this balance can be altered, leading to shifts in the Earth’s climate patterns. Most significant are the 11-year solar cycles that include periods of both increased and decreased solar activity. During periods of heightened solar activity, the total solar irradiance (TSI) can increase, which can have moderate impacts on the Earth’s climate.

An increase in TSI can cause warming at the Earth’s surface, leading to a rise in global average temperatures. This phenomenon, known as solar forcing, contributes to natural climate variability. However, solar forcing is not the primary driver of the current global warming trend, as the marked increase in temperatures over the past century is primarily attributed to anthropogenic greenhouse gas emissions. Nonetheless, variations in solar radiation can influence regional climate patterns, such as through changes in atmospheric circulation, impacts on monsoon systems, and modulation of sea surface temperatures.

While the link between solar radiation and Earth’s climate has been well-established, there are still uncertainties in understanding precisely how these relationships function. Some proposed climate feedback mechanisms include the influence of solar radiation on cloud cover and stratospheric ozone concentrations, both of which can alter the balance of solar energy absorbed and reflected by the Earth.

Geomagnetic Storms and Space Weather

Distinct from its effects on terrestrial weather and climate, solar radiation also plays a role in shaping space weather. When solar activity is high, the sun emits streams of charged particles known as solar wind, which carries a magnetic field that can interact with the Earth’s magnetosphere. This interaction can cause geomagnetic storms, disruptions in the Earth’s magnetic field generated by the transfer of energy from the solar wind to the magnetosphere. Geomagnetic storms can have harmful consequences for electrical power systems, navigation systems, and satellites, and are known to produce stunning displays of the aurora borealis and aurora australis.

High-energy solar events such as solar flares, CMEs, and high-speed solar wind streams can create more intense geomagnetic storms. The risks associated with these storms include the induction of electric currents in power lines and transformers, which can lead to power grid failures or blackouts. Additionally, the high levels of ionizing radiation generated during a geomagnetic storm can pose hazards to astronauts and aircraft on polar flight routes.

Effects on Satellite Communications

Changes in solar radiation can also impact satellite communications, as high-energy solar events can cause damage to satellites and disrupt their functionality. During solar flares and CMEs, the sun emits streams of high-energy particles and radiation that can penetrate satellite shielding and damage sensitive electronic components. This radiation can induce a buildup of electric charge within a satellite, which can eventually result in an electrostatic discharge that damages critical systems.

High levels of solar radiation can also cause disruptions to the Earth’s ionosphere, the region of the atmosphere that is ionized by solar radiation and consists mostly of free electrons and ions. Changes in ionospheric conditions can lead to degradation in satellite communication signals, resulting in errors or complete signal loss. This impact on satellite communications is particularly concerning as our society becomes increasingly reliant on satellite-based technologies, including global positioning systems (GPS), communication, and weather monitoring.

Biological Effects and UV Radiation

Finally, variations in solar radiation can have biological effects on Earth, particularly through changes in ultraviolet (UV) radiation levels. UV radiation is harmful to living organisms, as it can damage DNA, proteins, and other key cellular components. An excess of UV exposure can lead to skin cancer, cataracts, and immune system dysfunction in humans, as well as harm to ecosystems and crop yields.

The Earth’s ozone layer plays a crucial role in protecting life on our planet from harmful UV radiation by absorbing much of it before it reaches the ground. While variations in solar radiation can impact this ozone layer, it is important to note that the primary cause of recent ozone depletion has been the release of chlorofluorocarbons (CFCs) and other ozone-depleting substances (ODS) by human activities. However, understanding the interaction between solar radiation and atmospheric chemistry is essential for accurate climate modeling and predicting the future impacts of changes in solar output on ozone levels and UV exposure.

Monitoring, Measurement, and Predictions

Monitoring, measurement, and predictions of solar activities are essential for understanding and predicting the Sun’s impact on Earth’s climate, telecommunications, and electrical grids. Comprehensive monitoring methods, advanced forecasting techniques, and ongoing research efforts help scientists develop insights into the Sun’s behavior and its interactions with our planet. This section highlights an overview of techniques and tools for solar observation, modeling and forecasting solar cycles, and current and future research directions.

Techniques and Tools for Observation

Observing the Sun requires a range of tools and techniques capable of capturing crucial information on solar activities. Some of the primary techniques and tools for solar observation include:

  1. Ground-based observatories: Ground-based solar observatories house telescopes with specialized filters to focus on specific wavelengths of light, allowing scientists to study features such as sunspots, solar flares, and coronal mass ejections. Some examples include the National Solar Observatory in the United States and the Observatorio del Teide in Spain.
  2. Space-based observatories: These observatories are placed in orbit around the Earth to observe and study the Sun without interference from the Earth’s atmosphere. Notable space-based solar observatories include the Solar and Heliospheric Observatory (SOHO), the Solar Dynamics Observatory (SDO), and the Parker Solar Probe.
  3. Radio telescopes: Radio telescopes detect solar radio emissions and provide valuable insights into the Sun’s magnetic fields and coronal mass ejections. Some examples of radio telescopes used for solar observations are the Nobeyama Radio Observatory in Japan and the Owens Valley Radio Observatory in the United States.
  4. Spectroscopy: This technique involves splitting light into its various wavelengths to reveal information about the chemical composition, temperature, and magnetic fields of the solar atmosphere. Spectroscopy is used in both ground-based and space-based instruments, such as the Hinode satellite and the Swedish Solar Telescope.

Modeling and Forecasting Solar Cycles

Solar cycles are the regular fluctuations in the Sun’s activity, typically characterized by the rise and fall in the number of sunspots. Solar cycles usually last about 11 years and predicting the timing and intensity of these cycles is essential for anticipating space weather events that can have significant effects on Earth.

Several models are used to forecast solar cycles, including:

  1. Empirical models: These models rely on historical patterns and statistical analyses of previous solar cycles. Empirical models are relatively simple but can provide valuable insights into the general progression of solar cycles.
  2. Dynamo models: Dynamo models simulate the complex interactions between solar magnetic fields and fluid motions inside the Sun. These models can provide detailed forecasting of solar cycle characteristics, such as the timing of cycle maxima and minima, and the emergence of sunspots.
  3. Data assimilation models: These models merge observational data and numerical simulations to predict the evolution of solar magnetic fields and subsequent solar activities. They can be useful in estimating the solar cycle’s strength and other relevant features.

Current and Future Research

Continuous monitoring and advancements in solar observation techniques have provided a wealth of data and insights into the Sun’s behavior. Current research focuses on improving the understanding and forecasting of solar cycles, space weather events, and their impacts on Earth.

Some areas of ongoing research include:

  1. Magnetohydrodynamic (MHD) simulations: MHD simulations model the behavior of plasma in the Sun’s interior and atmosphere, allowing scientists to study the Sun’s magnetic field and its relation to various solar activities.
  2. Space weather modeling: Developing accurate models to predict the impact of solar activities on the Earth’s magnetosphere and ionosphere is crucial for mitigating potential negative effects on our technology and infrastructure.
  3. Solar-terrestrial interactions: Understanding the complex interactions between solar activities and Earth’s climate and weather systems is an area of ongoing research. This knowledge can help improve our ability to predict and respond to the potential impacts of solar cycles on our planet.

As our understanding of the Sun’s behavior and its interactions with Earth continues to improve, researchers will develop more accurate and reliable models to predict solar cycles and potential space weather events, providing essential information for policymakers and operators of critical systems worldwide.

Frequently Asked Questions

1. What is a solar cycle and how does it influence solar radiation levels?

A solar cycle is a roughly 11-year cycle of changes in the Sun’s activity, marked by an increase or decrease in sunspots and solar flares. Solar radiation levels vary as a result of these fluctuations, affecting the Earth’s climate and the performance of solar energy systems.

2. How do sunspots and solar flares impact solar radiation?

Sunspots are cooler, magnetically active areas on the Sun’s surface, while solar flares are bursts of radiation and energy. Both phenomena can release additional radiation and charged particles, influencing the overall level of solar radiation reaching Earth.

3. What is the connection between the solar cycle and Earth’s climate?

The solar cycle’s impact on solar radiation levels can affect Earth’s climate by causing temperature variations and altering atmospheric circulation patterns. The influence may be subtle, but it is crucial to understand when studying climate change.

4. How can understanding solar cycles benefit solar energy systems?

Knowledge about solar cycles enables improved prediction of solar radiation levels, allowing for more accurate planning and design of solar energy systems. This information helps maximize efficiency and ensures reliable energy production during both peak and low solar activity periods.

5. Does solar activity pose any risks to satellite systems and grid infrastructure?

Yes, heightened solar activity, such as coronal mass ejections, can produce geomagnetic storms that impact satellite-based communication and navigation systems. Power grids can also be affected; understanding solar cycles helps mitigate these risks through preparedness and technological adaptation.

6. How has tracking and prediction of solar cycles improved over time?

Advancements in solar observation, satellite technology, and computer modeling have improved our ability to track and predict solar cycles. This ongoing research offers valuable insights into the Sun’s behavior and its implications for solar radiation levels and climate on Earth.


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