Human Realm

The Mortal Plane (Art by Pablo Carlos Budassi)

### Aliases

Mortal Realm, Earth Realm, Midgard, Ecumene, Assiah, Universe, Frontrooms, Earthrealm, Material World, Overworld, Realm of Mortals, World of the Senses, Observable Universe

## Details

### Located within

World Tree

The **Human Realm** is one of the first realms to ever exist, lasting for nearly 14 billion years, and as far as most are concerned, the realm should continue to exist for billions of years more.

## History

### Before Universe

What was there before the creation of the universe is and perhaps always will be a mystery to both humanity and most angels. All that is known is that before there was light, a terrible war was waged for the domination of the universe between God and the Arcuthas against the Abyssal Gods. God was the ruler of light, good and order, and gathered in itself all that was good, all that was fair and luminous.

### The Big Bang

After the War of Creation, God created the singularity, and in that singularity, within a moment or so, exploded. After that moment, all distances throughout the universe began to increase from zero because the it changed over time, affecting distances between all non-bound objects everywhere. For this reason it is said that the Big Bang "happened everywhere".

### The very early universe

Distances between celestial objects in the cosmos have continuously grown since the inception of the Big Bang, persisting to this day. This expansion is particularly noticeable in unbound regions, except for gravitationally bound objects like galaxies and many clusters, where the pace of expansion notably diminished. During the inflationary period, the expansion experienced a rapid acceleration. Subsequent to inflation, and for approximately 9.8 billion years, the expansion rate notably decelerated and continued to do so progressively (albeit never reversing). Approximately 3 billion years later, there was a subtle resurgence in the pace of expansion.

#### Planck epoch

In this epoch, the temperature and average energies within the universe were sufficiently high that everyday subatomic particles could not coalesce, and even the four fundamental forces that govern the universe — gravitation, electromagnetism, the weak nuclear force, and the strong nuclear force — merged to constitute a single fundamental force.

#### Grand unification epoch

As the universe expanded and cooled, it traversed specific transition temperatures at which the fundamental forces dissociated from their unified state. These phase transitions can be likened to the condensation and freezing processes of ordinary matter. At particular temperatures or energies, much like how water molecules alter their behavior and structure when transitioning from steam to water, the fields governing our universe's fundamental forces and particles also undergo profound changes when the temperature or energy drops below a certain threshold.

This transformation isn't discernible in our everyday experiences because it occurs at significantly higher temperatures than those encountered in our current universe.

The grand unification epoch commenced with one such phase transition, marking the separation of gravity from the all-encompassing gauge force. This division resulted in the existence of two distinct forces: gravity and an electro-strong interaction. The grand unification epoch drew to a close with a subsequent phase transition, as the electro-strong interaction itself underwent separation, giving rise to two independent interactions known as the strong and electroweak interactions.

#### Electroweak epoch

The electroweak epoch commenced a mere 10^-36 seconds following the Big Bang, as the universe's temperature had decreased sufficiently for the electronuclear force to segregate into two distinct interactions: the strong and electroweak interactions.

During the inflationary epoch, a momentous transformation occurred in the very early universe. The metric governing spatial distance abruptly and dramatically altered in scale, resulting in the universe expanding to a volume at least 10^78 times its previous size. Although the speed of light remains an upper limit for the movement of light and objects within spacetime, in this scenario, it was the metric that characterizes the size and geometry of spacetime itself that underwent a substantial change in scale.

This profound transformation was instigated by the separation of the strong and electroweak interactions, which marked the conclusion of the grand unification epoch. As the inflation field settled into its lowest energy state throughout the universe, it generated an immense repulsive force, triggering a rapid expansion of the spatial metric itself.

The swift expansion of space resulted in the dispersion of elementary particles that had persisted since the grand unification epoch, scattering them thinly throughout the universe. However, the substantial potential energy of the inflation field was released as the inflaton field decayed into other particles, a phenomenon known as "reheating." This reheating process reintroduced a dense, hot mixture of quarks, anti-quarks, and gluons into the universe. In some models, reheating is often considered the starting point of the electroweak epoch, and certain theories, such as warm inflation, circumvent the need for a reheating phase entirely.

Inflation concluded at a temperature corresponding to approximately 10^-32 seconds after the Big Bang, but this doesn't imply that the inflationary era lasted less than 10^-32 seconds. Following the end of inflation, the universe continued to expand, albeit at a considerably slower pace. Approximately 4 billion years ago, the expansion gradually began to accelerate once again. Consequently, the masses of particles and their superpartners were no longer equal.

#### Electroweak symmetry breaking

As the temperature of the universe dropped to approximately 159.5±1.5 GeV, a significant event known as electroweak symmetry breaking occurred. This event represented one of the crucial symmetry-breaking events in the formation of our universe, with the ultimate one being chiral symmetry breaking in the quark sector. Electroweak symmetry breaking had two interconnected effects. Firstly, all elementary particles that interacted with the Higgs field became massive, having previously been massless at higher energy levels. Secondly, the weak nuclear force, electromagnetic force, and their respective bosons (the W and Z bosons and photon) began to exhibit distinct behaviors in the evolving universe. Before electroweak symmetry breaking, these bosons were all massless particles, capable of interacting over long distances. However, following this event, the W and Z bosons acquired mass, becoming particles that could only interact over distances smaller than the size of an atom, while the photon remained massless and continued to mediate long-distance interactions.

Following electroweak symmetry breaking, the fundamental interactions took on their contemporary forms, and fundamental particles acquired the expected masses. However, the universe's temperature remained too high to permit the stable formation of many of the particles we currently observe in the universe. Consequently, there were no protons or neutrons, and thus no atoms, atomic nuclei, or molecules at this stage.

### The early universe

Following the conclusion of cosmic inflation, the universe is populated by a hot quark-gluon plasma, which is the residual product of the reheating process. Starting from this stage onward, the physics of the early universe becomes considerably more comprehensible, and the energies associated with the Quark epoch are directly accessible through particle physics experiments and various detectors. This provides scientists with the means to probe and study the fundamental processes and particles that characterize this phase of the universe's history.

#### The quark epoch

The quark epoch commenced approximately 10^-12 seconds following the Big Bang. This phase in the early universe's evolution followed immediately after electroweak symmetry breaking, during which the fundamental interactions of gravitation, electromagnetism, the strong interaction, and the weak interaction had assumed their current forms. However, the temperature of the universe remained too high during this epoch to allow quarks to combine and form hadrons.

Throughout the quark epoch, the universe was brimming with a dense, hot quark-gluon plasma, containing quarks, leptons, and their corresponding antiparticles. Collisions between particles were exceedingly energetic, preventing quarks from coalescing into mesons or baryons.

The quark epoch drew to a close when the universe was approximately 10^-5 seconds old, at a point when the average energy of particle interactions had dropped below the mass of the lightest hadron, the pion.

##### Baryogenesis

Baryons, which include particles like protons and neutrons, are subatomic particles composed of three quarks. Under normal expectations, one would anticipate that baryons and their counterparts known as antibaryons would have formed in roughly equal quantities in the early universe. However, this appears not to be the case, and as far as we know, the universe contains a significantly greater number of baryons compared to antibaryons. In fact, very few antibaryons are observed in nature. The exact reason for this imbalance remains unclear.

Explaining this phenomenon requires satisfying the Sakharov conditions related to baryogenesis, a process responsible for generating the excess baryons, which must have occurred at some point after the conclusion of cosmological inflation. Current particle physics theories suggest the existence of certain asymmetries that could meet these conditions. However, these asymmetries, as currently understood, appear to be too small to account for the substantial observed imbalance between baryons and antibaryons in the universe. This intriguing puzzle remains a subject of ongoing research and exploration within the field of particle physics and cosmology.

#### Hadron epoch

As the quark-gluon plasma that comprised the early universe cooled down, it reached a point where hadrons, including baryons like protons and neutrons, could begin to form. Initially, pairs of hadrons and their corresponding antiparticles could coexist, and matter and antimatter were in thermal equilibrium. However, as the universe's temperature continued to decrease, the creation of new hadron-antihadron pairs ceased, and most of the newly formed hadrons and antihadrons annihilated each other. This annihilation process resulted in the generation of pairs of high-energy photons. A relatively small residue of hadrons persisted until approximately 1 second of cosmic time, marking the conclusion of this epoch.

According to theoretical predictions, there was approximately one neutron for every six protons, and this ratio gradually shifted to about 1:7 due to neutron decay over time. This prediction aligns with observations because, at a later stage, some of the neutrons and protons combined through nuclear fusion, resulting in the formation of hydrogen, a hydrogen isotope called deuterium, helium, and other elements. These elements can be measured and observed, and a 1:7 ratio of hadrons would indeed produce the observed element ratios in both the early and current universe.

#### Neutrino decoupling and cosmic neutrino background (CνB)

Approximately 1 second after the Big Bang, neutrinos decoupled from other particles and began to travel freely through space. Neutrinos have a very low interaction rate with matter, which allows them to persist in the universe to this day, akin to the cosmic microwave background (CMB) radiation, which was emitted during the recombination period about 370,000 years after the Big Bang. The neutrinos produced during this event possess extremely low energy, around 10 times smaller than what can be detected with current technology. Even high-energy neutrinos are notoriously challenging to detect, which makes the direct observation of the cosmic neutrino background (CνB) a complex and ongoing task, with potential observations still far on the horizon.

Nevertheless, the framework of Big Bang cosmology generates numerous predictions regarding the CνB, and there is compelling indirect evidence for its existence. This evidence is derived from Big Bang nucleosynthesis predictions of the abundance of helium in the universe and from observations of anisotropies in the cosmic microwave background (CMB). One such prediction is that neutrinos should have left a subtle imprint on the CMB. The CMB exhibits irregularities, with some fluctuations having a nearly regular spacing due to baryonic acoustic oscillations. In theory, the decoupled neutrinos should have caused a subtle shift in the phase of various CMB fluctuations.

In 2015, it was reported that such shifts had indeed been detected in the CMB. These fluctuations in the CMB corresponded to neutrinos with a temperature very close to the value predicted by Big Bang theory (1.96 ± 0.02K, compared to the prediction of 1.95K), and precisely matched the existence of three distinct types of neutrino flavors, which is in line with the number of neutrino flavors anticipated by the Standard Model of particle physics. This discovery provides strong support for the existence of the cosmic neutrino background and the overall framework of Big Bang cosmology.

#### Possible formation of primordial black holes

Primordial black holes are a theoretical type of black hole proposed in 1966 as a potential consequence of the early universe's high densities and inhomogeneous conditions during the radiation-dominated era. They may have formed within the first second of cosmic time due to random fluctuations that led to certain regions becoming dense enough to undergo gravitational collapse, ultimately giving rise to black holes. However, current scientific knowledge and theories place stringent limits on the abundance and mass of these hypothetical objects.

Typically, the formation of primordial black holes would require density contrasts, which are regional variations in the universe's density, of approximately 10% compared to the average density of the universe. There are various mechanisms that could lead to the creation of sufficiently dense regions meeting this criterion during the early universe, including processes like reheating, cosmological phase transitions, and, in the context of "hybrid inflation models," axion inflation. One notable feature of primordial black holes is that they did not originate from the gravitational collapse of massive stars, allowing for a wide range of possible masses, which can be much lower than typical stellar black holes (around 2×10^33 grams).

In fact, Stephen Hawking's calculations in 1971 suggested that primordial black holes could have extremely low masses, potentially as light as 10^-5 grams. Additionally, these primordial black holes could vary in size, with some being significantly larger. The existence of primordial black holes, regardless of their mass, is an intriguing aspect of cosmological theory, and they are considered a potential contributor to the formation of galaxies and other cosmic structures. However, direct observational evidence for their existence remains elusive, and further research is ongoing in this area of astrophysics and cosmology.

#### Lepton epoch

At the conclusion of the hadron epoch, the majority of hadrons and anti-hadrons annihilate each other, resulting in the prevalence of leptons (including electrons, muons, and certain neutrinos) and their antiparticles in the universe, dominating the mass content.

The lepton epoch follows a pattern similar to the preceding hadron epoch. Initially, leptons and antileptons are generated in pairs. However, about 10 seconds after the Big Bang, as the temperature of the universe continues to decrease, the conditions become less conducive to the formation of new lepton-antilepton pairs. Consequently, most of the remaining leptons and antileptons quickly annihilate each other, producing pairs of high-energy photons. This annihilation process leaves behind only a small residue of non-annihilated leptons.

#### Photon epoch

At the conclusion of the lepton epoch, following the annihilation of most leptons and antileptons, the predominant form of mass-energy in the universe consists of photons. The remaining mass-energy is composed of neutrinos and other relativistic particles. Consequently, the energy and overall dynamics of the universe are primarily governed by photons during this period.

These photons continue to interact frequently with charged particles, such as electrons, protons, and eventually, atomic nuclei. This interaction persists for approximately the next 370,000 years, during which time the universe undergoes various transformations and transitions, eventually leading to the formation of atoms and the cosmic microwave background radiation.

#### Nucleosynthesis of light elements

Between approximately 2 and 20 minutes after the Big Bang, the conditions in the universe were conducive to nuclear fusion, a process known as "Big Bang nucleosynthesis." During this relatively short time span, the high temperature and pressure in the early universe enabled the formation of atomic nuclei, primarily consisting of a few light elements beyond hydrogen.

Around 25% of the protons and all of the neutrons present underwent fusion reactions, resulting in the formation of deuterium, which is a hydrogen isotope. Most of the deuterium nuclei subsequently fused to create helium-4, the most abundant isotope of helium. This process of nuclear fusion during the early moments of the universe was responsible for the generation of these light elements and laid the foundational framework for the chemical composition of the cosmos.

#### Matter domination

Up to this point, the large-scale dynamics and behavior of the universe have been primarily influenced by radiation, which includes constituents that move at relativistic speeds, such as photons and neutrinos. As the universe continues to cool, which occurs around 47,000 years after the Big Bang (corresponding to a redshift z = 3600), the universe's large-scale behavior undergoes a transition, and it becomes dominated by matter instead. This shift happens because the energy density of matter starts to surpass both the energy density of radiation and the vacuum energy density.

At or shortly after approximately 47,000 years, the energy densities of non-relativistic matter, primarily composed of atomic nuclei, and relativistic radiation, predominantly photons, become equal. This equilibrium marks an important turning point in the evolution of the universe. It signifies that the Jeans length, which dictates the smallest structures that can form, begins to decrease. The Jeans length determines these structures by balancing the competing effects of gravitational attraction and pressure. As a result of this transition, perturbations in the universe's density, instead of being wiped out by the free streaming of radiation, can now commence their growth in amplitude. This phase is pivotal for the formation of larger structures in the universe, including galaxies and galaxy clusters, as gravitational forces can now overcome the effects of pressure, allowing these perturbations to evolve and condense.

#### First molecules

The behavior of dark matter in the universe is fundamentally different from that of ordinary matter because of its unique properties. Dark matter possesses characteristics that enable it to collapse quickly due to gravitational interactions, unhindered by radiation pressure. However, these same properties also mean that dark matter cannot lose energy through radiation, as normal matter does. The loss of energy is a critical factor that allows particles to collapse further into dense structures. As dark matter cannot shed energy through radiation, it cannot condense into stars, planets, or other compact, radiating objects.

Instead, dark matter tends to collapse into vast but diffuse structures, forming the framework for the large-scale cosmic web of filaments and massive haloes that encapsulate galaxies. These dark matter haloes serve as gravitational scaffolding around which ordinary matter can gather and eventually lead to the formation of galaxies. In contrast, ordinary matter, which can efficiently lose energy through radiation processes, can condense into dense objects such as stars and planets, as well as form gas clouds when it collapses.

The different behaviors of dark matter and ordinary matter are integral to our understanding of the universe's structure and evolution, with dark matter playing a pivotal role in the formation of large-scale cosmic structures, while ordinary matter gives rise to the smaller, more familiar objects like stars and planets.

#### Recombination, photon decoupling, and the cosmic microwave background (CMB)

About 370,000 years after the Big Bang, two significant events took place: recombination and photon decoupling. Recombination refers to the process where ionized particles combine to form the first neutral atoms, while decoupling describes the release ("decoupling") of photons as the newly formed atoms settle into more stable energy states.

Just before recombination, the baryonic matter in the universe was at a temperature where it existed as a hot ionized plasma. During this phase, most of the photons in the universe interacted with electrons and protons and could not travel significant distances without repeatedly interacting with these ionized particles. Consequently, the universe was opaque or "foggy" during this period. Although there was light, it was not possible to see, nor could we observe that light through telescopes or other instruments, due to the continuous scattering and absorption of photons by the ionized particles. This era is often referred to as the "cosmic fog."

### The Dark Ages and large-scale structure emergence.

*Around 370,000 to roughly 1 billion years following the occurrence of the Big Bang.*

#### Dark Ages

Following recombination and decoupling, the universe entered a phase in which it became transparent and cooled sufficiently to permit the travel of light over long distances. However, during this period, there were no light-emitting structures such as stars and galaxies. Stars and galaxies are formed through the gravitational collapse of dense gas regions, a process that occurs slowly in the presence of relatively uniform gas density. It's estimated that stars didn't come into existence until hundreds of millions of years after recombination.

This era, known as the Dark Ages, commenced around 370,000 years after the Big Bang. Over this time, the universe's temperature dropped from about 4000 K to roughly 60 K (3727 °C to about −213 °C). Only two sources of photons were present during the Dark Ages: the photons released during recombination/decoupling (when neutral hydrogen atoms formed), which we can still detect today as the cosmic microwave background (CMB), and sporadic photons emitted by neutral hydrogen atoms, referred to as the 21 cm spin line of neutral hydrogen. This hydrogen spin line falls within the microwave frequency range, and within 3 million years, the CMB photons shifted from visible light to infrared. During this period, until the first stars emerged, there were no visible light photons, except for possibly some infrequent statistical anomalies, rendering the universe predominantly dark.

The first generation of stars, known as Population III stars, came into being within several hundred million years after the Big Bang. These stars represented the initial source of visible light in the universe after recombination. Structures might have begun to form around 150 million years, and early galaxies emerged between 380 and 700 million years. While there are no separate observations of very early individual stars (the earliest stars are identified within very early galaxies), their formation marked the gradual end of the Dark Ages. This transition was gradual, and the Dark Ages only fully concluded around 1 billion years after the Big Bang, shaping the universe's appearance as we recognize it today.

Additionally, there is an ongoing observational effort aimed at detecting the faint 21 cm spin line radiation. In principle, this radiation offers a potent means of studying the early universe, even more so than the cosmic microwave background.

##### Speculative "habitable epoch"

For approximately 6.6 million years, spanning from around 10 to 17 million years after the Big Bang (corresponding to a redshift range of 137 to 100), the background temperature of the universe ranged from 273 to 373 K (0 to 100 °C). This temperature range is conducive to the existence of liquid water and the occurrence of common biological chemical reactions. In 2014, Abraham Loeb proposed the intriguing concept that primitive life could, in theory, have emerged during this specific time frame, which he termed the "habitable epoch of the early Universe."

Loeb's speculation revolves around the idea that carbon-based life might have developed within a hypothetical region of the early universe that possessed the necessary conditions. This region would have had to be both dense enough to give rise to at least one massive star, which would later release carbon through a supernova explosion, and also dense enough to generate a planet. It's important to note that such dense pockets, if they did exist, would have been exceptionally rare in the early universe.

In addition to density conditions, the emergence of life would have required a heat differential, rather than just a uniform background radiation. This differential could have been supplied by naturally occurring geothermal energy sources. However, any life that might have evolved during this period would likely have remained in a primitive state. The timespan during the habitable epoch of the early Universe was relatively short, making it highly improbable for intelligent life to evolve within that timeframe. Additionally, the epoch would have culminated with the freezing over of any hypothetical oceans, further limiting the prospects for the persistence and development of life beyond its primitive stages.

#### Earliest structures and stars emerge

The composition of the universe consists of approximately 84.5% cold dark matter and 15.5% "ordinary" matter. Since the onset of the matter-dominated era, dark matter has been gradually coalescing into vast, widespread filaments, influenced by the force of gravity. In contrast, ordinary matter eventually congregates more rapidly than it would have on its own, thanks to the presence of these concentrations of dark matter. Moreover, ordinary matter is somewhat denser at regular intervals due to early baryon acoustic oscillations (BAO), which became ingrained in the distribution of matter when photons decoupled.

Unlike dark matter, ordinary matter has various means to lose energy. This characteristic allows it to dissipate the energy that would otherwise keep its particles apart, causing it to collapse more swiftly and into denser forms. Ordinary matter comes together in regions where dark matter is denser, forming clouds predominantly composed of hydrogen gas. It is within these clouds that the first stars and galaxies take shape.

As these galaxies multiply, galaxy clusters and superclusters eventually emerge. Large voids, sparsely populated by stars, develop in the spaces between these cosmic structures. These voids serve as markers, indicating areas where dark matter is less abundant. This intricate interplay between dark matter and ordinary matter has played a pivotal role in shaping the large-scale structure of the universe.

#### Reionization

The formation of the first stars, dwarf galaxies, and quasars leads to the emission of intense radiation. This radiation has the effect of reionizing a significant portion of the surrounding universe. Reionization is the process by which neutral hydrogen atoms are split back into a plasma composed of free electrons and protons. This marks the first time this has occurred since the period of recombination and decoupling.

The evidence for reionization primarily comes from observations of quasars. Quasars are a type of active galaxy and are among the most luminous objects observed in the universe. Neutral hydrogen atoms have specific patterns of absorbing photons, which are related to electron energy levels and are known as the Lyman series.

In contrast, ionized hydrogen lacks electron energy levels of this nature. Consequently, when light travels through ionized hydrogen and neutral hydrogen, it exhibits different absorption lines. These distinct absorption line patterns observed in quasars and other astronomical objects provide a clear indication of the reionization process and the transition of the universe from a predominantly neutral state to a plasma of ionized particles.

#### Galaxies, clusters and superclusters

Matter continues to coalesce under the relentless pull of gravity, leading to the formation of galaxies. The stars that emerge during this phase are referred to as Population II stars and are among the earliest to form. Population I stars, which are more recent, come into existence at later stages of this process.

Additionally, the gravitational attraction among galaxies gradually causes them to move closer to one another, leading to the formation of groups, clusters, and superclusters of galaxies. Observations from the Hubble Ultra Deep Field have revealed instances of smaller galaxies merging to create larger ones. Some of these merger events are dated to around 800 million years into cosmic time, roughly 13 billion years ago. However, it's worth noting that the accuracy of this age estimate has been subject to refinement and may have been slightly overestimated in earlier assessments. The ongoing process of galaxy formation and evolution continues to be a significant area of study in cosmology and astrophysics.

## Myths and Legends

Many cultures have stories describing the origin of the world and universe. Cultures generally regard these stories as having some truth. There are however many differing beliefs in how these stories apply amongst those believing in a supernatural origin, ranging from a god directly creating the universe as it is now to a god just setting the "wheels in motion" (for example via mechanisms such as the big bang and evolution).

Ethnologists and anthropologists who study myths have developed various classification schemes for the various themes that appear in creation stories. For example, in one type of story, the world is born from a world egg; such stories include the Finnish epic poem *Kalevala*, the Chinese story of Pangu or the Indian Brahmanda Purana. In related stories, the universe is created by a single entity emanating or producing something by him- or herself, as in the Tibetan Buddhism concept of Adi-Buddha, the ancient Greek story of Gaia (Mother Earth), the Aztec goddess Coatlicue myth, the ancient Egyptian god Atum story, and the Judeo-Christian Genesis creation narrative in which the Abrahamic God created the universe. In another type of story, the universe is created from the union of male and female deities, as in the Maori story of Rangi and Papa. In other stories, the universe is created by crafting it from pre-existing materials, such as the corpse of a dead god—as from Tiamat in the Babylonian epic *Enuma Elish* or from the giant Ymir in Norse mythology—or from chaotic materials, as in Izanagi and Izanami in Japanese mythology. In other stories, the universe emanates from fundamental principles, such as Brahman and Prakrti, the creation myth of the Serers, or the yin and yang of the Tao.

## Locations

* Sun: The star at the center of the entire realm.
* Mercury: The smallest and innermost planet named after the roman deity.
* Venus: The second-brightest natural object in the night sky after the Moon named after the deity.
* Earth: The most populated planet, containing humans and animals.
* Mars: A red planet named after the roman deity, it supposedly contains Martians.
* Jupiter: A gas giant with a mass one-thousandth that of the Sun named after the roman deity.
* Saturn: A gas giant with an average radius of about nine times that of Earth named after the roman deity.
* Uranus: The seventh planet from the Sun.
* Neptune: The fourth-largest planet by diameter named after the roman deity.
* Pluto: A dwarf planet in the Kuiper belt named after the roman deity.
* Nibiru: The home world of the Anunnaki.
* Yuggoth: A planet located at the very edge of the Solar System.
* Planet Popstar: A distant planet shaped like a yellow five-pointed star.
* Ripple Star: Home planet of the fairies.
* Halcandra: The original homeworld of "The Ancients."
* Theia: An ancient planet that collided with Earth billions of years ago.

## Trivia

* Although the universe is thought to be black, if the universe were viewed outside of a dark environment, its color would be beige, a rather pale beige, similar to the color of a latte - and that's why scientists called this tone "coffee with cosmic milk".