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Hubble's Nebulae Hubble telescope discovered some nebulae here is an image and detail of the nebulae and other information about it. Emission Nebulae Emission nebulae are so named because they emit their own light. This type of nebula forms when the intense radiation of stars within or near the nebula energizes the gas. A star’s ultraviolet radiation floods the gas with so much energy that it strips electrons from the nebula’s hydrogen atoms, a process called ionization. As the energized electrons revert from their higher-energy state to a lower-energy state by recombining with atoms, they emit energy in the form of light, causing the nebula’s gas to glow. A famous example of an emission nebula is the Orion Nebula, a huge, star-forming nebula in the constellation Orion. The Orion Nebula is home to a star cluster defined by four massive stars known as the Trapezium. These stars are only a few hundred thousand years old, about 15-30 times the mass of the Sun, and so hot and bright that they’re responsible for illuminating the entire Orion nebula. But thousands of additional, mostly young stars are embedded in the nebula. The most massive are 50 to 100 times the mass of our Sun. The radiation and solar winds of stars within emission nebulae carve and sculpt the nebula’s gas, creating caverns and pillars but also creating pressures on the gas clouds that can give rise to more starbirth. Reflection Nebulae Reflection nebulae reflect the light from nearby stars. The stars that illuminate them aren’t powerful enough to ionize the nebula’s gas, as with emission nebulae, but their light scatters through the gas and dust causing it to glow ― like a flashlight beam shining on mist in the dark. Because of the way light scatters when it hits the fine dust of the interstellar medium, these reflection nebulae are often bluish in color. A reflection nebula called NGC 1999 lies close to the famous Orion Nebula, about 1,500 light-years from Earth. The nebula is illuminated by a bright, recently formed star called V380 Orionis, and the gas and dust of the nebula is material left over from that star’s formation. A second well-known reflection nebula is illuminated by the Pleiades star cluster. Most nebulae around star clusters consist of material that the stars formed from. But the Pleiades shines on an independent cloud of gas and dust, drifting through the cluster at about 6.8 miles/second (11 km/s). Planetary Nebulae When astronomers looked at the sky through early telescopes, they found many indistinct, cloudy forms. They called such objects “nebulae,” Latin for clouds. Some of the fuzzy objects resembled planets, and these earned the name “planetary nebulae.” Today these nebulae keep the name, but we know they have nothing to do with planets. Planetary nebulae form during the death of low-mass to medium-mass stars. When such stars die, they expel their outer layers into space. These expanding shells of gas form a huge variety of unique shapes ― rings, hourglasses, rectangles, and more ― that show the complexity of stellar death. Astronomers are still studying how these intricate shapes form at the end of a star’s life. As the star casts off its outer layers, it leaves behind its core, which becomes a white dwarf star. White dwarf stars are objects with the approximate mass of the Sun but the size of Earth, making them one of the densest forms of matter in the universe after black holes and neutron stars. The white dwarf star’s ultraviolet radiation ionizes the gas of the planetary nebula and causes it to glow, just as stars do in emission nebulae. Our Sun is expected to form a planetary nebula at the end of its life. Crab Nebula Not all stars die gently, exhaling their outer layers into space. Some explode in a supernova, flinging their contents into space at anywhere from 9,000 to 25,000 miles (15,000 to 40,000 kilometers) per second. When a star has a lot of mass ― at least five times that of our Sun ― or is part of a binary system in which a white dwarf star can gravitationally pull mass from a companion star, it can explode with the brightness of 10 billion Suns. Supernova remnants consist of material from the exploded star and any interstellar material it sweeps up in its path. The new debris from the explosion and material ejected by the star earlier in its life collide, heating up in the shock until it glows with x-rays. Supernova remnants’ glow can also be powered by the stellar wind of a pulsar ― a rapidly spinning neutron star created from the core of the exploded star. The pulsar emits electrons that interact with the magnetic field it produces, a process called synchrotron radiation, and emits X-rays, visible light and radio waves. The Crab Nebula is an example of a supernova remnant. The explosion that created it in the year 1054 was so bright that for weeks it could be seen even in the daytime sky, and it was recorded by astronomers across the world. The material from the star is still rushing outward at around 3 million mph (4.8 million kph). Absorption Nebulae Absorption nebulae or dark nebulae are clouds of gas and dust that don’t emit or reflect light, but block light coming from behind them. These nebulae tend to contain large amounts of dust, which allows them to absorb visible light from stars or nebulae beyond them. Astronomer William Herschel, discussing these seemingly empty spots in the late 1700s, called them “a hole in the sky.” Included among absorption nebulae are objects like Bok globules, small, cold clouds of gas and dense cosmic dust. Some Bok globules have been found to have warm cores, which would be caused by star formation inside, and further observation has indicated the presence of multiple stars of varying ages, suggesting a slow, ongoing star formation process. Hubble's Nebulae Gallery

KEPLER-452b Kepler-452b, often referred to as "Earth's cousin," is an exoplanet that was discovered by NASA's Kepler Space Telescope. It was announced as a significant discovery in July 2015. Here's a detailed explanation of Kepler-452b, including information about its characteristics, atmosphere, and the potential for extraterrestrial life 1. Characteristics of Kepler-452b: Size and Mass: Kepler-452b is considered a super-Earth, as it is larger than Earth, with an estimated radius about 1.6 times that of Earth. However, its exact mass is still uncertain, as it depends on its composition, which is not precisely known. Orbit: Kepler-452b orbits a star known as Kepler-452, which is very similar to our Sun in terms of both size and temperature. Its orbit around Kepler-452 takes approximately 385 days, making it roughly analogous to Earth's year. Distance from Star: Kepler-452b is located within the habitable zone of its parent star. The habitable zone, also known as the "Goldilocks zone," is the region around a star where conditions may be right for liquid water to exist on the planet's surface—a key factor for the potential development of life as we know it. Age: The host star Kepler-452 is older than our Sun, estimated to be around 6 billion years old, which could have allowed more time for life to potentially develop on Kepler-452b. 2. Atmosphere of Kepler-452b: The exact composition and characteristics of Kepler-452b's atmosphere are not currently known. The detection and analysis of exoplanet atmospheres are challenging tasks and often require advanced instruments like the James Webb Space Telescope (scheduled for launch) to provide more detailed information. The presence and composition of an atmosphere are critical factors in determining the potential habitability of an exoplanet. An atmosphere can help regulate temperature, protect against harmful radiation, and play a role in supporting life processes. 3. Potential for Extraterrestrial Life: Kepler-452b's location within the habitable zone of its star makes it an intriguing candidate for the potential existence of extraterrestrial life. The habitable zone represents the region where conditions might be suitable for liquid water, a fundamental ingredient for life as we know it, to exist on the planet's surface. However, the presence of liquid water alone does not guarantee the existence of life. Many other factors, such as the planet's atmosphere, geological activity, and the availability of essential chemical ingredients, would also influence its habitability. Detecting signs of life on Kepler-452b or any exoplanet is extremely challenging and would likely require advanced telescopes capable of analyzing the planet's atmosphere for biomarkers (e.g., oxygen and methane) or other potential signs of biological activity. Kepler-452b and Earth are both planets, but they have some significant differences, as well as similarities. Here's a comparison between the two: 1. Size and Mass: Earth: Earth is approximately 12,742 kilometers (7,918 miles) in diameter and has a mass of about 5.972 × 10^24 kilograms. Kepler-452b: Kepler-452b is estimated to be about 1.6 times the size (radius) of Earth, but its mass is not precisely known. It's considered a super-Earth. 2. Orbit and Parent Star: Earth: Earth orbits the Sun, a G-type main-sequence star (G2V), at an average distance of about 149.6 million kilometers (93 million miles). Kepler-452b: Kepler-452b orbits a G-type main-sequence star (G2V) known as Kepler-452, which is very similar to the Sun. Its orbital period is approximately 385 Earth days. 3. Habitability and Atmosphere: Earth: Earth has a diverse and life-sustaining atmosphere composed primarily of nitrogen (78%) and oxygen (21%), with trace amounts of other gases. It has liquid water on its surface and a stable climate, making it highly habitable. Kepler-452b: The exact composition of Kepler-452b's atmosphere is not known, and its habitability is still uncertain. It's located within the habitable zone of its star, indicating the potential for liquid water, but more information about its atmosphere is needed to assess its suitability for life. 4. Age: Earth: Earth is approximately 4.5 billion years old. Kepler-452b: The host star Kepler-452 is estimated to be about 6 billion years old, making it older than the Sun. This could have implications for the potential development of life on the planet. 5. Surface Conditions: Earth: Earth has a diverse range of surface conditions, including continents, oceans, and various climate zones. It supports a wide variety of life forms and ecosystems. Kepler-452b: The specific surface conditions of Kepler-452b, such as the presence of oceans or continents, are not known due to limited observational data. 6. Potential for Extraterrestrial Life: Earth: Earth is known to host a vast array of life, from microorganisms to complex multicellular organisms, including humans. Kepler-452b: Kepler-452b is considered a potentially habitable exoplanet due to its location within the habitable zone, but the presence of extraterrestrial life on the planet is purely speculative at this point. More research and observations are needed to assess its habitability and the potential for life. Other Articles...... Dark Energy Multiness of Thoughts The Dream Mission Creation of Mind Loop STAR VFTS102 KEPLER-186f Proxima Centauri b TRAPPIST-1

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This program is about deep space knowledge we provides you a detail knowledge about a single corner of space by specific software and also a space exploration for intimate knowledge about space this is best program for you

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