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SN 1181
First observed between August 4 and August 6, 1181, Chinese and Japanese astronomers recorded the supernova now known as SN 1181 in eight separate texts. One of only nine supernovae in the Milky Way observable with the naked eye in recorded history, it appeared in the constellation Cassiopeia and was visible in the night sky for about 185 days. Pulsar 3C-58 The radio and X-ray pulsar J0205+6449 (also known as 3C 58), which rotates about 15 times per second, has been identified as the possible remnant from this event. If the supernova and pulsar are associated, the star is still rotating about as quickly as it did when it first formed. This is in contrast to the Crab pulsar, known to be the remnant of the SN 1054 supernova in the year 1054, which has lost two-thirds of its rotational energy in essentially the same time span. A paper of radio surveys of 3C 58 published in 2006 indicated that this supernova remnant may be much older and thus not associated with SN 1181. However ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
3C 58
3C 58 or 3C58 is a pulsar (designation PSR J0205+6449) and supernova remnant (pulsar wind nebula) within the Milky Way that is possibly associated with the supernova of 1181. There are, however, signs that indicate that it could be several thousand years old, and thus not associated with that supernova. The object is listed as No. 58 in the Third Cambridge Catalogue of Radio Sources. The pulsar is notable for its very high rate of cooling, which is unexplained by standard theories of neutron star formation. It is hypothesized that extreme conditions in the star's interior cause a high neutrino flux, which carries away the energy so that the star cools. 3C 58 has been proposed as a possible quark star. It is located 2° northeast of ε Cassiopeiae and is estimated to be 10,000 light-years away. Its rotation period is 65.7 ms (so PSR J0205+6449 does not belong to the class of millisecond pulsar A millisecond pulsar (MSP) is a pulsar with a rotational peri ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Parker's Star
The Smith's Snackfood Company is a British-Australian snack food company owned by American multinational corporation PepsiCo. It is best known for its brand of potato crisps. The company was founded by Frank Smith and Jim Viney in the United Kingdom in 1920 as Smiths Potato Crisps Ltd, originally packaging a twist of salt with its crisps in greaseproof paper bags which were sold around London. The dominant brand in the UK until the 1960s when Edinburgh's Golden Wonder took over with Cheese & Onion, Smith’s countered by creating Salt & Vinegar flavour (first tested by their north-east England subsidiary Tudor) which was launched nationally in 1967. After establishing the product in the UK, Smith set up the company in Australia in 1932. PepsiCo acquired a controlling stake in 1998. Smith's Snackvend Stand is the branch of the company that operates vending machines. Smiths by country United Kingdom Smith's Potato Crisps Ltd. was formed by Frank Smith and Jim Viney in the Unit ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
1181
Year 1181 ( MCLXXXI) was a common year starting on Thursday (link will display the full calendar) of the Julian calendar. Events By place Europe * King Philip II (Augustus) annuls all loans made by Jews to Christians, and takes a percentage for himself. A year later, he confiscates all Jewish property and expels the Jews from Paris. * Philip II begins a war against Philip of Alsace, count of Flanders, over the Vermandois. He claims the territory for his wife Isabella of Hainault as her dowry. Philip is unwilling to give it up. * Henry the Lion, duke of Saxony, submits to Emperor Frederick I (Barbarossa) at an Imperial Diet in Erfurt. He is banished to England and retains only Brunswick among his former lands. * King Béla III of Hungary and Croatia goes to war with Venice in an effort to recover Dalmatia. The city of Zadar (located on the Adriatic Sea) accepts Béla's suzerainty. * After a series of defeats, the Almohad fleet under the admiral Ahmad al-Siqilli, cr ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
12th Century In Science
1 (one, unit, unity) is a number representing a single or the only entity. 1 is also a numerical digit and represents a single unit of counting or measurement. For example, a line segment of ''unit length'' is a line segment of length 1. In conventions of sign where zero is considered neither positive nor negative, 1 is the first and smallest positive integer. It is also sometimes considered the first of the infinite sequence of natural numbers, followed by 2, although by other definitions 1 is the second natural number, following 0. The fundamental mathematical property of 1 is to be a multiplicative identity, meaning that any number multiplied by 1 equals the same number. Most if not all properties of 1 can be deduced from this. In advanced mathematics, a multiplicative identity is often denoted 1, even if it is not a number. 1 is by convention not considered a prime number; this was not universally accepted until the mid-20th century. Additionally, 1 is the s ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Supernova Remnants
A supernova remnant (SNR) is the structure resulting from the explosion of a star in a supernova. The supernova remnant is bounded by an expanding shock wave, and consists of ejected material expanding from the explosion, and the interstellar material it sweeps up and shocks along the way. There are two common routes to a supernova: either a massive star may run out of fuel, ceasing to generate fusion energy in its core, and collapsing inward under the force of its own gravity to form a neutron star or a black hole; or a white dwarf star may accrete material from a companion star until it reaches a critical mass and undergoes a thermonuclear explosion. In either case, the resulting supernova explosion expels much or all of the stellar material with velocities as much as 10% the speed of light (or approximately 30,000 km/s). These speeds are highly supersonic, so a strong shock wave forms ahead of the ejecta. That heats the upstream plasma up to temperatures well above milli ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Supernova Remnants
This is a list of observed supernova remnants (SNRs) in the Milky Way, as well as galaxies nearby enough to resolve individual nebulae, such as the Large Magellanic Cloud, Large and Small Magellanic Clouds and the Andromeda Galaxy. Supernova remnants typically only survive for a few tens of thousands of years, making all known SNRs fairly young compared to many other astronomical objects. See also *List of supernovae *Supernova *Lists of astronomical objects References External linksList of all known (extra)galactic supernova remnantsaThe Open Supernova Catalog {{DEFAULTSORT:List Of Supernova Remnants Lists of nebulae, Supernova Remnants Supernova remnants, * Light sources, Supernova Remnants, list of Articles containing video clips ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Supernovae
This is a list of supernovae that are of historical significance. These include supernovae that were observed prior to the availability of photography, and individual events that have been the subject of a scientific paper that contributed to supernova theory. An alternative, complete and updated list can be found in thOpen Supernova Catalog List ''In most entries, the year when the supernova was seen is part of the designation (1st column).'' See also * List of most distant supernovae * List of supernova candidates * List of supernova remnants * Lists of astronomical objects References Further reading * External linksList of all known supernovaeaThe Open Supernova CatalogIAU Supernovaeon thTransient Name Server (TNS) at IAU |
Guest Star (astronomy)
In Chinese astronomy, a guest star () is a star which has suddenly appeared in a place where no star had previously been observed and becomes invisible again after some time. The term is a literal translation from ancient Chinese astronomical records. Modern astronomy recognizes that guest stars are manifestations of cataclysmic variable stars: novae and supernovae. The term "guest star" is used in the context of ancient records, since the exact classification of an astronomical event in question is based on interpretations of old records, including inference, rather than on direct observations. In ancient Chinese astronomy, guest stars were one of the three types of highly transient objects (bright heavenly bodies). The other two were comets with tails () and comets without tails (), with the former term being used for all comets in modern astronomy. The earliest Chinese record of guest stars is contained in ''Han Shu'' (漢書), the history of Han Dynasty (206 BC – A ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Zombie Star
A zombie star is a hypothetical result of a Type Iax supernova which leaves behind a remnant star, rather than completely dispersing the stellar mass. Type Iax supernovae are similar to Type Ia, but have a lower ejection velocity and lower luminosity. Type Iax supernovae may occur at a rate between 5 and 30 percent of the Ia supernova rate. Thirty supernovae have been identified in this category. In a binary system consisting of a white dwarf and a companion star, the white dwarf strips away material from its companion. Normally the white dwarf would eventually reach a critical mass, and fusion reactions would make it explode and completely dissipate it, but in a Type Iax supernova, only half of the dwarf's mass is lost. Observed instances Supernova SN 2012Z in the NGC 1309 galaxy is thought to be of type Iax, and was discovered by S.B. Cenko, W. Li, and A.V. Filippenko using the Katzman Automatic Imaging Telescope on 2012 January 29.15 UT as part of a supernova ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Type Iax Supernova
A Type Ia supernova (read: "type one-A") is a type of supernova that occurs in binary systems (two stars orbiting one another) in which one of the stars is a white dwarf. The other star can be anything from a giant star to an even smaller white dwarf. Physically, carbon–oxygen white dwarfs with a low rate of rotation are limited to below 1.44 solar masses (). Beyond this "critical mass", they reignite and in some cases trigger a supernova explosion; this critical mass is often referred to as the Chandrasekhar mass, but is marginally different from the absolute Chandrasekhar limit, where electron degeneracy pressure is unable to prevent catastrophic collapse. If a white dwarf gradually accretes mass from a binary companion, or merges with a second white dwarf, the general hypothesis is that a white dwarf's core will reach the ignition temperature for carbon fusion as it approaches the Chandrasekhar mass. Within a few seconds of initiation of nuclear fusion, a substantial ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Parsecs
The parsec (symbol: pc) is a unit of length used to measure the large distances to astronomical objects outside the Solar System, approximately equal to or (au), i.e. . The parsec unit is obtained by the use of parallax and trigonometry, and is defined as the distance at which 1 au subtends an angle of one arcsecond ( of a degree). This corresponds to astronomical units, i.e. 1\, \mathrm = 1/\tan \left( \ \mathrm \right)\, \mathrm. The nearest star, Proxima Centauri, is about from the Sun. Most stars visible to the naked eye are within a few hundred parsecs of the Sun, with the most distant at a few thousand. The word ''parsec'' is a portmanteau of "parallax of one second" and was coined by the British astronomer Herbert Hall Turner in 1913 to make calculations of astronomical distances from only raw observational data easy for astronomers. Partly for this reason, it is the unit preferred in astronomy and astrophysics, though the light-year remains prominent in pop ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
IRAS 00500+6713
IRAS 00500+6713 is a type of star announced in December 2020 and created by the explosive merger of two ultra-dense white dwarfs. It consists of a super-hot central star, a super-Chandrasekhar object with a mass ≳1.5 M⊙ called J005311, surrounded by a nebula packed with hot gas and warm dust. The star represents a new kind of X-ray source. It exhibits record-breaking wind speeds and large amounts of neon, magnesium, silicon, and sulfur. It has been linked to the supernova SN 1181. The star is highly unstable, too massive to remain as a white dwarf, and it is predicted to collapse into a neutron star A neutron star is the collapsed core of a massive supergiant star, which had a total mass of between 10 and 25 solar masses, possibly more if the star was especially metal-rich. Except for black holes and some hypothetical objects (e.g. white ... within ten thousand years. References Compact stars Cassiopeia (constellation) IRAS catalogue objects {{star ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
