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Jennie McCormick
Jennie Margaret McCormick , FRASNZ (; born 1963) is a New Zealand amateur astronomer and asteroid discoverer who conducts astronomical research from the Farm Cove Observatory in Auckland. She discovered the asteroid officially named New Zealand and has contributed to and been involved in a range of organisations and events to promote astronomy. McCormick has published in several journals and won awards for her contributions to astronomy. Early life and education McCormick was born in and grew up in Whanganui and attended Whanganui Girls' College. Her family moved to Auckland when she was 15. Initially she worked in a stable with racehorses, but at the age of 29, after attending a lecture at the Stardome in Auckland, McCormick joined the Auckland Astronomical Society (AAS), which introduced her to "like-minded amateur astronomers and academics". Career Since 2002 she has been the sole proprietor of Farm Cove Observatory, an observatory in Pakuranga, a suburb of Auckland. The ob ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Jennie McCormick 21 May 2020
{{disambiguation ...
Jennie may refer to: * Jennie (singer), South Korean singer of girl group Blackpink * Jennie, a female given name, variant spelling of Jenny * ''Jennie'' (musical), 1963 Broadway production * ''Jennie'' (novel), 1994 science fiction thriller by Douglas Preston * ''Jennie'' (film), a 1940 American drama film * Jennie, Georgia, a community in the United States See also * Jenni * Jenny (other) Jenny may refer to: * Jenny (given name), a popular feminine name and list of real and fictional people * Jenny (surname), a family name Animals * Jenny (donkey), a female donkey * Jenny (gorilla), the oldest gorilla in captivity at the time of ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Astronomers Without Borders
Astronomers Without Borders (AWB) is a U.S.-based organization founded by Mike Simmons, dedicated to spreading astronomy throughout the world and connecting people through this universal interest. Projects include crowdfunding in developed countries to sponsor the purchase of equipment and training for people in developing countries. The group's aim is to create "goodwill and understanding" across all boundaries through the sharing of astronomy. The group was founded in 2007, and achieved official tax-free status in 2009, which was the International Year of Astronomy (IYA2009). AWB sponsored several events that year, including The World At Night (TWAN), and assisted in the IYA2009's Global Cornerstone Project 100 Hours of Astronomy. Utilizing important historical and natural settings across the globe, The World at Night created wide-angle images of the sky, in order to show the universality of star-gazing. 100 Hours of Astronomy ran April 2–5, 2009, the goal of which was to get ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Intermediate Polars
In astronomy, an intermediate polar (also called a DQ Herculis Star) is a type of cataclysmic variable, binary star system with a white dwarf and a cool main-sequence secondary star. In most cataclysmic variables, matter from the companion star is gravitationally stripped by the compact star and forms an accretion disk around it. In intermediate polar systems, the same general scenario applies except that the inner disk is disrupted by the magnetic field of the white dwarf. The name "intermediate polar" is derived from the strength of the white dwarf's magnetic field, which is between that of non-magnetic cataclysmic variable systems and strongly magnetic systems. Non-magnetic systems exhibit full accretion disks, while strongly magnetic systems (called polars or AM Herculis systems) exhibit only accretion streams which directly impact the white dwarf's magnetosphere. There were 26 confirmed intermediate polar systems as of 14 April 2006. This represents about 1% of the 1,8 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
T Pyxidis
T Pyxidis (''T Pyx'') is a recurrent nova and nova remnant in the constellation Pyxis. It is a binary star system and its distance is estimated at about from Earth. It contains a Sun-like star and a white dwarf. Because of their close proximity and the larger mass of the white dwarf, the latter draws matter from the larger, less massive star. The influx of matter on the white dwarf's surface causes periodic thermonuclear explosions to occur. The usual apparent magnitude of this star system is 15.5, but there have been observed eruptions with maximal apparent magnitude of about 7.0 in the years 1890, 1902, 1920, 1944, 1966 and 2011. Evidence seems to indicate that T Pyxidis may have increased in mass despite the nova eruptions, and is now close to the Chandrasekhar limit when it might explode as a supernova. When a white dwarf reaches this limit it will collapse under its own weight and cause a type Ia supernova. Effect on Earth Because of its relative proximity, so ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Atomic Orbital
In atomic theory and quantum mechanics, an atomic orbital is a function describing the location and wave-like behavior of an electron in an atom. This function can be used to calculate the probability of finding any electron of an atom in any specific region around the atom's nucleus. The term ''atomic orbital'' may also refer to the physical region or space where the electron can be calculated to be present, as predicted by the particular mathematical form of the orbital. Each orbital in an atom is characterized by a set of values of the three quantum numbers , , and , which respectively correspond to the electron's energy, angular momentum, and an angular momentum vector component (magnetic quantum number). Alternative to the magnetic quantum number, the orbitals are often labeled by the associated harmonic polynomials (e.g., ''xy'', ). Each such orbital can be occupied by a maximum of two electrons, each with its own projection of spin m_s. The simple names s orbital, p orb ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Photometry (astronomy)
Photometry, from Greek '' photo-'' ("light") and '' -metry'' ("measure"), is a technique used in astronomy that is concerned with measuring the flux or intensity of light radiated by astronomical objects. This light is measured through a telescope using a photometer, often made using electronic devices such as a CCD photometer or a photoelectric photometer that converts light into an electric current by the photoelectric effect. When calibrated against standard stars (or other light sources) of known intensity and colour, photometers can measure the brightness or apparent magnitude of celestial objects. The methods used to perform photometry depend on the wavelength region under study. At its most basic, photometry is conducted by gathering light and passing it through specialized photometric optical bandpass filters, and then capturing and recording the light energy with a photosensitive instrument. Standard sets of passbands (called a photometric system) are defined to allow a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Corvidae
Corvidae is a cosmopolitan family of oscine passerine birds that contains the crows, ravens, rooks, jackdaws, jays, magpies, treepies, choughs, and nutcrackers. In colloquial English, they are known as the crow family or corvids. Currently, 133 species are included in this family. The genus ''Corvus'', including the crows, rooks, and ravens, makes up over a third of the entire family. Corvids (ravens) are the largest passerines. Corvids display remarkable intelligence for animals of their size, and are among the most intelligent birds thus far studied. Specifically, members of the family have demonstrated self-awareness in mirror tests (European magpies) and tool-making ability (e.g. crows and rooks), skills which until recently were thought to be possessed only by humans and a few other higher mammals. Their total brain-to-body mass ratio is equal to that of non-human great apes and cetaceans, and only slightly lower than that of humans.Birding in India and South AsiaCor ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
OGLE-2005-BLG-071L
OGLE-2005-BLG-071L is a distant, magnitude 19.5 galactic bulge star located in the constellation Scorpius, approximately 11,000 light years away from the Solar System. The star is probably a red dwarf with a mass 43% of that of the Sun. Planetary system In 2005 an exoplanet was discovered orbiting this star by the microlensing method, the second planet found by this method. The planet was later confirmed by the Keck telescope and its properties were refined. See also * List of extrasolar planets * Optical Gravitational Lensing Experiment The Optical Gravitational Lensing Experiment (OGLE) is a Polish astronomical project based at the University of Warsaw that runs a long-term variability sky survey (1992–present). The main goals are the detection and classification of variable ... or ''OGLE'' References External links * M-type main-sequence stars Scorpius (constellation) Planetary systems with one confirmed planet Gravitational lensing {{ ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Exoplanet
An exoplanet or extrasolar planet is a planet outside the Solar System. The first possible evidence of an exoplanet was noted in 1917 but was not recognized as such. The first confirmation of detection occurred in 1992. A different planet, initially detected in 1988, was confirmed in 2003. There are many methods of detecting exoplanets. Transit photometry and Doppler spectroscopy have found the most, but these methods suffer from a clear observational bias favoring the detection of planets near the star; thus, 85% of the exoplanets detected are inside the tidal locking zone. In several cases, multiple planets have been observed around a star. About 1 in 5 Sun-like starsFor the purpose of this 1 in 5 statistic, "Sun-like" means G-type star. Data for Sun-like stars was not available so this statistic is an extrapolation from data about K-type stars. have an "Earth-sized"For the purpose of this 1 in 5 statistic, Earth-sized means 1–2 Earth radii. planet in the habitable zone. ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Orbital Period
The orbital period (also revolution period) is the amount of time a given astronomical object takes to complete one orbit around another object. In astronomy, it usually applies to planets or asteroids orbiting the Sun, moons orbiting planets, exoplanets orbiting other stars, or binary stars. For celestial objects in general, the sidereal period ( sidereal year) is referred to by the orbital period, determined by a 360° revolution of one body around its primary, e.g. Earth around the Sun, relative to the fixed stars projected in the sky. Orbital periods can be defined in several ways. The tropical period is more particularly about the position of the parent star. It is the basis for the solar year, and respectively the calendar year. The synodic period incorporates not only the orbital relation to the parent star, but also to other celestial objects, making it not a mere different approach to the orbit of an object around its parent, but a period of orbital relations ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Cataclysmic Variable Star
In astronomy, cataclysmic variable stars (CVs) are stars which irregularly increase in brightness by a large factor, then drop back down to a quiescent state. They were initially called novae (), since ones with an outburst brightness visible to the naked eye and an invisible quiescent brightness appeared as new stars in the sky. Cataclysmic variable stars are binary stars that consist of two components; a white dwarf primary, and a mass transferring secondary. The stars are so close to each other that the gravity of the white dwarf distorts the secondary, and the white dwarf accretes matter from the companion. The tightest currently observed orbit in a hydrogen-rich system is 51 minutes in ZTF J1813+4251. Therefore, the secondary is often referred to as the ''donor star''. The infalling matter, which is usually rich in hydrogen, forms in most cases an accretion disk around the white dwarf. Strong UV and X-ray emission is often seen from the accretion disc, powered by the loss ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Superhump
In astronomy, a superhump is a periodic brightness variation in a cataclysmic variable star system, with a period within a few percent of the orbital period of the system. History Superhumps were first seen in SU Ursae Majoris (SU UMa) stars, a subclass of dwarf novae, at times when the binary system underwent a superoutburst, which is an unusually strong outburst (increase in brightness) caused by an increased accretion rate. Period excess The period of the superhump variations can be either greater or less than the orbital period, known as positive or negative superhumps respectively. The period excess is the difference between the superhump period and the orbital period, expressed as a fraction of the orbital period. Physical origin The accretion disk is elongated by the tidal force of the donor star. The elliptical disk precesses around the white dwarf accretor over a time interval much longer than the orbital period, the beat period, causing a slight change in the orien ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
