1537News Space Weather

WHAT IS SPACE WEATHER?

Our Sun is a really active star. It does all sorts of things that send out energy and tiny particles. These things are called solar flares and coronal mass ejections. When these happen, they create what we call "Space Weather." This is all about how the space around Earth changes because of the energy and particles from the Sun. This can affect our planet and the things we use in our daily lives.
So, what are the effects of this space weather? Well, it can cause problems like satellites going wonky, issues with communication and navigation in airplanes, and even dangers to astronauts in space. Sometimes, satellites can even get pulled back to Earth because of the changes in space. Plus, big space storms from the Sun can mess with our electrical power at home and work. So, understanding space weather is really important.

But wait, how can there be "weather" in space? After all, space is mostly empty, like a super-duper vacuum. Earth's air is way thicker than space. For example, if you're near sea level on Earth, there are a whole lot of air molecules in every tiny bit of space - about 2 followed by 19 zeroes of them! That's like 1.2 kilograms of air in each cubic meter. But when you get far above our planet, like 500 kilometers (300 miles), it's really, really thin up there, with hardly any air. The solar wind, which is the stuff coming from the Sun, only has 1 to 10 particles in each cubic centimeter as it passes by Earth. So, it's super different from the air we eathe on Earth.

Schumann Resonance is like a special hum that the Earth makes. It's not something we can hear with our ears, but it's there all the time. Imagine you have a big drum, and you hit it softly. The drum will make a deep sound that you can feel more than hear. That's a bit like the Schumann Resonance, which is like the Earth's drumbeat.

The Earth is like a giant battery, and it has a special layer around it called the ionosphere. This layer is full of electrically charged particles, and they sometimes get zapped by lightning during thunderstorms. When this happens, it sends out energy waves into the Earth. These waves move very fast, like when you drop a pebble into a pond, and ripples spread out.

What is the Schumann Resonance?

The Schumann Resonance is the name for the waves that bounce between the Earth's surface and the ionosphere. These waves are super important because they help all living things on Earth, including us, feel better and stay healthy. It's like a natural heartbeat for our planet.

Scientists have measured the Schumann Resonance, and it usually viates at around 7.83 times per second. This is a very low hum, and it's so low that we can't hear it. But many people think that our bodies and minds can feel this viation, and it helps us be balanced and relaxed.

In summary, the Schumann Resonance is like the Earth's secret hum, a natural rhythm that keeps our planet in balance. It's always there, even if we can't hear it, and it might have a positive impact on how we feel and stay healthy. So, even though we can't see or hear it, the Schumann Resonance is still an essential part of our world.

Schumann Resonance

Dependence of frequencies of the Schumann resonance in hertz on the local time

Local time is expressed in hours of Tomsk Daylight Saving Time (TLDV).TLDV=UTC+7hours.

Dependences of Schumann resonance amplitudes on local time. Local time is Tomsk Daylight Saving Time(TLDV)|TLDV=UTC+7hours.

Amplitudes Dependences of Schumann resonance amplitudes on local time.
Local time is expressed in hours of Tomsk Daylight Saving Time (TLDV). TLDV=UTC+7hours.

Dependences of Schumann resonance amplitudes on local time.
Local time is Tomsk Daylight Saving Time (TLDV)|TLDV=UTC+7hours.

Quality Factors: Dependences of the quality factors of the Schumann resonance on local time.

Local time is Tomsk Daylight Saving Time (TLDV). TLDV=UTC+7hours.

Critical Frequencies:
Dependences of the critical frequencies of the ionosphere on local time. Local time is Tomsk Daylight Saving Time (TLDV).
TLDV=UTC+7hours.

Critical frequencies Dependences of the critical frequencies of the ionosphere on local time.
Local time is expressed in hours of Tomsk Daylight Saving Time (TLDV). TLDV=UTC+7hours.

Critical frequencies without sporadic layers:
Dependences of the critical frequencies of the ionosphere on local time.

Local time is expressed in hours of Tomsk Daylight Saving Time (TLDV).
TLDV=UTC+7hours.

Active Heights:
Dependences of the actual heights of the ionosphere on local time.

Local time is Tomsk Daylight Saving Time (TLDV).
TLDV=UTC+7hours.

Dependences of the actual heights of the ionosphere on local time.
Local time is Tomsk Daylight Saving Time (TLDV).
TLDV=UTC+7hours.">

Raw data provided by the National Geophysical Data Center NGDC. On a 9-point scale, an estimate of the foF2 parameter of the world base is given in terms of the volume and homogeneity of data in a number of experimental values for each ionospheric station. Based on the degree of database filling, the total number of stations (224 pieces) represents 9 groups with a radius proportional to the degree of filling (in the 1st group there are 8 stations, in the 2nd - 10 stations, in the 3rd - 11, in the 4th - 12, in the 5th - 14, in the 6th - 18, in the 7th - 22, in the 8th - 34, and in the 9th group - 95 stations).">

Raw data provided by the National Geophysical Data Center NGDC.

Our Dynamic Sun

AIA 304 Å - Solar Region: Transition Region_Chromosphere Emitted by helium-2 (He II) at temperatures around 50,000 Kelvin. This light is emitted from the chromosphere and transition region SDO images of this wavelength are typically colorized in red. Credit: NASA/SDO/Goddard

AIA 131 Å - Solar Region: Corona_Flaring Regions Emitted by iron-20 (Fe XX) and iron-23 (Fe XXIII) At temperatures greater than 10,000,000 Kelvin, representing the material in flares. The images are typically colorized in teal. Credit: NASA/SDO/Goddard

AIA 193 Å - Solar Region: Corona_Flare Plasma Emitted by iron-12 (Fe XII) at 1,000,000 K and iron 24 (Fe XXIV) At temperatures of 20,000,000 Kelvin. The former, Iron-20 represents a slightly hotter region of the corona The latter, iron-16 represents the much hotter material of a solar flare. This wavelength is typically colorized in light brown. Credit: NASA/SDO/Goddard

AIA 335 Å - Solar Region: Corona_Active Regions Emitted by iron-16 (Fe XVI) At temperatures of 2,500,000 Kelvin. These images also show hotter, magnetically active regions in the corona. This wavelength is typically colorized in blue. Credit: NASA/SDO/Goddard

AIA 171 Å - Solar Region: Upper Transition Region_Quiet Corona Emitted by iron-9 (Fe IX) at around 600,000 Kelvin. This wavelength shows the quiet corona and coronal loops and is typically colorized in gold. Credit: NASA/SDO/Goddard

AIA 094 Å - Solar Region: Corona_Flaring Regions Emitted by iron-18 (Fe XVIII) At temperatures of 6,000,000 Kelvin. Temperatures like this represent regions of the corona during a solar flare. The images are typically colorized in green. Credit: NASA/SDO/Goddard

AIA 211 Å - Solar Region: Corona_Active Regions Emitted by iron-14 (Fe XIV) At temperatures of 2,000,000 Kelvin. These images show hotter, magnetically active regions in the sun's corona The images are typically colorized in purple. Credit: NASA/SDO/Goddard

This movie is generated for a wavelength of 1600 Ångstroms (160.0 nanometers) which highlights a spectral line of carbon that has lost 3 electrons (also known as carbon-4 or C-IV) at temperatures of 10,000 K. C IV at these temperatures is present in what's called the transition region between the sun's surface and the lowest levels of the sun's atmosphere, the chromosphere.

AIA 1700 Å - Solar Region: Photosphere_Chromosphere Ultraviolet light continuum, shows the surface of the sun, as well as a layer of the sun's atmosphere called the chromosphere, which lies just above the photosphere and is where the temperature begins rising. SDO images of this wavelength are typically colorized in a grainy pink. Temperatures: 4,500-5,000 Kelvin. Credit: NASA/SDO/Goddard

AIA 4500 Å - Solar Region: Photosphere White light continuum, shows the sun's surface or photosphere in visible light; Continuums provide photographs of the solar surface, incorporating a oad range of visible light in the temperature range of 5,000-6,000 Kelvin and appears in ight yellow. Credit: NASA/SDO/Goddard

The magnetogram image shows the magnetic field in the solar photosphere, with black and white indicating opposite polarities.

The Helioseismic and Magnetic Imager (HMI) is a scientific research instrument that studies changes in the Sun's magnetic field. It takes images of the Sun in polarized light every 50 seconds. [3] The HMI is aboard the SDO, which takes images of the solar photosphere in a narrow range of visible light wavelengths every 45 seconds. The HMI observes the entire solar disk at 6173 Å with a resolution of 1 arcsecond.