Let’s Talk Radio-Isotopes and Miyake Events and Energies

stock here: One of the arguments people use to refute a certain Miyake event is that they don’t have corresponding Be-10 isotopes. Higher energy events may have a predominance of C-14 and much less Be-10. Its a world few have travelled into.

what is the relation between carbon-14 formation in the atmosphere and BE-10 and the suspected solar events related to such. Also could gamma ray bursts from other stars reach here with enough concentration to significantly change the C-14 and B-10 in the atmosphere

ChatGPT

The formation of carbon-14 (C-14) and beryllium-10 (Be-10) in the Earth’s atmosphere is primarily influenced by cosmic rays, which are high-energy particles originating from various sources, including the sun and other celestial bodies. Both C-14 and Be-10 are isotopes that are produced when cosmic rays interact with nitrogen and oxygen in the atmosphere.

The relationship between C-14 and Be-10 is that they are both cosmogenic isotopes, meaning their production is initiated by cosmic rays. However, the specific processes leading to the production of each isotope are different.

1. Carbon-14 (C-14):
   • C-14 is formed when cosmic rays collide with nitrogen-14 (N-14) in the atmosphere, resulting in the transformation of nitrogen into C-14. This radioactive isotope is then incorporated into carbon dioxide and enters the carbon cycle through processes such as photosynthesis.
2. Beryllium-10 (Be-10):
   • Be-10 is produced when cosmic rays interact with oxygen and nitrogen in the atmosphere. Nitrogen-14 and oxygen-16 are the main target nuclei for the production of Be-10. Once formed, Be-10 can be deposited on the Earth’s surface through precipitation.

Solar Events and Isotope Production:

• Solar events, such as solar flares and variations in solar activity, can influence the flux of cosmic rays reaching Earth. Changes in solar activity can potentially affect the production rates of C-14 and Be-10.
• For example, during periods of increased solar activity, the solar wind from the sun can have a shielding effect on cosmic rays, reducing their intensity reaching Earth. Conversely, during solar minimums, when solar activity is low, more cosmic rays can penetrate the atmosphere, potentially leading to higher production rates of cosmogenic isotopes.

Gamma Ray Bursts (GRBs) from Other Stars:

• Gamma-ray bursts are intense bursts of gamma-ray radiation that can originate from distant galaxies. While GRBs release an immense amount of energy, the likelihood of them significantly affecting C-14 and Be-10 levels on Earth is low.
• The Earth’s atmosphere provides substantial protection from cosmic rays and high-energy particles. Even though GRBs are powerful, the vast distances between stars and the Earth make it highly improbable for their impact to significantly alter the isotopic composition of the Earth’s atmosphere.

In summary, solar activity can influence the production rates of C-14 and Be-10 by modulating cosmic ray flux, but the impact of gamma-ray bursts from other stars on these isotopes is considered negligible due to the protective atmosphere and the vast distances involved.

how about a few discussions on how exactly the c-14 and Be-10 are created by the SEP from the sun, or is it highly magnetic plasmas, or it mostly due to a puffed up magnetic shield of earth mdulates GCRs downward and a quiet sun result in less puffed up earth shield and so the allowing more GCRs in which can then create the C-14 and BE-10ChatGPT

The creation of cosmogenic isotopes such as carbon-14 (C-14) and beryllium-10 (Be-10) is indeed influenced by solar activity and the interaction of galactic cosmic rays (GCRs) with the Earth’s atmosphere. Here are some discussions on how these isotopes are created:

1. Galactic Cosmic Rays (GCRs):
   • GCRs are high-energy particles, mostly protons and some heavier ions, that originate from outside our solar system. These cosmic rays continuously bombard the Earth. When GCRs collide with atoms in the Earth’s atmosphere, they can induce nuclear reactions, leading to the production of cosmogenic isotopes.
2. Solar Modulation:
   • Solar activity, particularly the solar wind and solar magnetic field strength, plays a crucial role in modulating the flux of GCRs reaching the Earth. During periods of high solar activity, the solar wind is stronger, and the sun’s magnetic field is more effective at deflecting cosmic rays away from the solar system. This can result in a reduction in the number of GCRs reaching the Earth.
   • Conversely, during solar minimums (periods of low solar activity), the solar wind weakens, and the sun’s magnetic shield is less effective. As a result, more cosmic rays can penetrate into the solar system and interact with the Earth’s atmosphere.
3. Formation of C-14 and Be-10:
   • Carbon-14 (C-14): The primary process leading to C-14 formation involves the interaction of cosmic rays with nitrogen-14 (N-14) in the Earth’s atmosphere. A neutron from the cosmic ray collides with N-14, transforming it into C-14. This newly formed C-14 then participates in the carbon cycle, becoming part of atmospheric carbon dioxide and subsequently incorporated into living organisms through processes like photosynthesis.
   • Beryllium-10 (Be-10): Be-10 is produced through the interaction of cosmic rays with oxygen and nitrogen in the atmosphere. Nitrogen-14 and oxygen-16 are common target nuclei for the production of Be-10. Once formed, Be-10 can be deposited on the Earth’s surface through precipitation.
4. Solar Energetic Particle (SEP) Events:
   • SEP events, associated with solar flares and coronal mass ejections (CMEs), can significantly enhance the flux of energetic particles, including protons, reaching the Earth. These events can contribute to the production of cosmogenic isotopes, including C-14 and Be-10, by increasing the number of energetic particles interacting with the atmosphere.

In summary, the modulation of cosmic rays by solar activity, specifically the solar wind and the sun’s magnetic field, plays a crucial role in the creation of cosmogenic isotopes in the Earth’s atmosphere. Solar minimums allow more cosmic rays to penetrate, contributing to the production of isotopes like C-14 and Be-10. SEP events can also enhance the flux of energetic particles, further influencing isotope production.

what are the relative particle energies needed to create c-14 and BE-10 respectivelyChatGPT

The creation of carbon-14 (C-14) and beryllium-10 (Be-10) involves cosmic rays interacting with elements in the Earth’s atmosphere, leading to nuclear reactions. The energy threshold for these reactions varies, but generally, they are in the range of tens of MeV (mega-electronvolts) or higher.

1. Carbon-14 (C-14) Formation:
   • The primary process for the formation of C-14 involves the interaction of cosmic rays with nitrogen-14 (N-14) in the Earth’s atmosphere. The reaction can be represented as follows: N-14+Cosmic Ray→C-14+ProtonN-14+Cosmic Ray→C-14+Proton
   • The energy threshold for this reaction is typically around 20 MeV or higher.
2. Beryllium-10 (Be-10) Formation:
   • Be-10 is produced when cosmic rays interact with oxygen and nitrogen in the atmosphere. The reaction involving nitrogen-14 can be expressed as: N-14+Cosmic Ray→Be-10+ProtonN-14+Cosmic Ray→Be-10+Proton
   • The energy threshold for the production of Be-10 is generally around 10-20 MeV.

Additionally, solar energetic particle (SEP) events, which are associated with solar flares and coronal mass ejections, can contribute to the production of cosmogenic isotopes. The energies of particles in SEP events can range from tens of keV (kilo-electronvolts) to several GeV, and they can play a role in the enhancement of C-14 and Be-10 production during such events.

I would hypothesize that most of c-14 produced is very high up in the atmosphere and therefore could take quite some time to mix all the way down to tree level, and also that cloud formation and rain as well as sprites could influence the rate of “grounding” the C-14ChatGPT

Several factors contribute to the transport and mixing of C-14 from the upper atmosphere to the Earth’s surface:

1. Atmospheric Mixing: Atmospheric circulation, including vertical and horizontal movements of air masses, helps distribute gases and particles throughout the atmosphere. While the upper atmosphere is where most cosmogenic isotopes are produced, these isotopes can gradually mix downward through atmospheric circulation.
2. Transport by Aerosols: Particles, including aerosols and fine particulate matter, can act as carriers for cosmogenic isotopes. These particles can facilitate the transport of C-14 from the upper atmosphere to lower levels.
3. Rain and Precipitation: Rainfall can play a significant role in bringing down C-14 from higher altitudes to the Earth’s surface. As raindrops form, they can capture atmospheric constituents, including C-14, and deposit them on the ground.
4. Cloud Formation: Clouds can influence the transport and deposition of atmospheric constituents, including C-14. Cloud droplets may contain C-14, and when the droplets collide and coalesce, they can fall to the surface as precipitation.
5. Sprites and Lightning: Transient luminous events such as sprites, which occur in the mesosphere and lower thermosphere, are associated with thunderstorms. These events might contribute to the downward transport of C-14 by influencing atmospheric processes in the upper layers.

However, it’s crucial to note that the overall concentration of C-14 at the Earth’s surface is also influenced by factors such as the rate of carbon exchange between the atmosphere and the biosphere (e.g., through photosynthesis in plants) and other biogeochemical processes.

Your hypothesis aligns with the understanding that the mixing and transport of cosmogenic isotopes are complex processes influenced by atmospheric dynamics, precipitation, and other meteorological phenomena. The specifics of these processes can be further studied through atmospheric and environmental science research.