<< < -he Haf hal har har He hea hel hel Her Her hid hig hip hom hor hot Hub Hug hur hyd hyd hyg hyp > >>
Hubble constant pâyâ-ye Hubble (#) Fr.: constante de Hubble |
Hubble Deep Field (HDF) meydân-e žarf-e Hubble (#) Fr.: champ profond de Hubble An image of a small region in the constellation → Ursa Major, based on the results of a series of observations by the → Hubble Space Telescope. The image was assembled from 342 separate exposures taken over ten consecutive days between December 18 and December 28, 1995. It covers an area 144 arcseconds across. |
Hubble diagram nemudâr-e Hubble (#) Fr.: diagramme de Hubble A plot of the → redshift of galaxies against their distance or against their → apparent magnitude. |
Hubble distance durâ-ye Hubble Fr.: distance de Hubble The distance from the Earth to the → cosmic horizon which marks the edge of the → observable Universe. Same as → Hubble radius, → Hubble length, and → cosmic horizon. |
Hubble flow tacân-e Hubble Fr.: flot de Hubble |
Hubble law qânun-e Hubble Fr.: loi de Hubble |
Hubble length derâzâ-ye Hubble Fr.: longueur de Hubble The distance traveled by light along a straight → geodesic in one → Hubble time. Also called the → Hubble radius, → Hubble distance, and → cosmic horizon. |
Hubble parameter pârânmun-e Hubble Fr.: paramètre de Hubble |
Hubble radius šo'â'-e Hubble (#) Fr.: rayon de Hubble The size of the observable Universe as derived from the ratio c/H_{0}, where H_{0} is the → Hubble-Lemaitre constant and c the → speed of light. Same as → Hubble distance, → Hubble length, and → cosmic horizon. |
Hubble sequence peyâye-ye Hubble Fr.: séquence de Hubble A classification scheme in which galaxies are ordered into a sequence based on their morphology. Same as the → Hubble classification. |
Hubble Space Telescope (HST) durbin-e fazâyi-ye Hubble, teleskop-e ~ ~ (#) Fr.: télescope spatial de Hubble A telescope of 2.4 m in diameter, a joint NASA and ESA project, launched in 1990 into a low-Earth orbit 600 km above the ground. It was equipped with a collection of several science instruments that worked across the entire optical spectrum (from infrared, through the visible, to ultraviolet light). During its lifetime Hubble has become one of the most important science projects ever. |
Hubble time zamân-e Hubble (#) Fr.: temps de Hubble An estimate for the age of the Universe by presuming that the Universe has always expanded at the same rate as it is expanding today. It is the inverse of the → Hubble-Lemaitre constant: t_{H} = 1/H_{0}. Also called the Hubble age or the Hubble period. |
Hubble-Lemaitre constant pâyâ-ye Hubble-Lemaître Fr.: constante de Hubble-Lemaître The → Hubble parameter for the → present epoch. It is the constant of proportionality between the → recession velocities of galaxies and their distances from each other. The latest determinations using the → Hubble Space Telescope observations of → Cepheids give H_{0} = 72 ± 8 km s^{-1} Mpc^{-1} (W. L. Freedman et al., 2001, ApJ 553, 47, arXiv:astro-ph/0012376), the → WMAP observations yield 70.4 ± 1.3 km s^{-1} Mpc^{-1} (N. Jarosik et al., 2011, ApJS 192, 14, arXiv:1001.4744), and the → Planck Satellite observations give 67.3 ± 1.2 km s^{-1} Mpc^{-1} (Planck Collaboration, 2014, A&A 571, A16, arXiv:1303.5076). More recently, the Hubble constant was derived by a team of astronomers, using the NASA/ESA Hubble Space Telescope, with a 2.4% accuracy (Adam G. Reiss et al., 2016, arXiv:1604.01424). The new value, 73.2 km s^{-1} Mpc^{-1}, suggests that the Universe is expanding between five and nine percent faster than previously calculated. The → Hubble law is only applicable for large distances (> 20 Mpc), when the proper motions of galaxies in groups and clusters cannot confuse the recession due to expansion. → Hubble; → Friedmann-Lemaitre Universe; → constant. |
Hubble-Lemaitre flow tacân-e Hubble-Lemaître Fr.: flot de Hubble-Lemaître The general outward motion of → galaxy clusters resulting from the → expansion of the Universe. → Hubble-Lemaitre law; → flow. |
Hubble-Lemaitre law qânun-e Hubble-Lamaître Fr.: loi de Hubble-Lemaître The speed with which a → galaxy cluster recedes from us is directly proportional to its distance. It can be stated as v = H_{0}d, where v is the recessional velocity, H_{0} the → Hubble-Lamaitre constant, and d the distance. See also → Hubble-Lemaitre flow. It should be underlined that Hubble was not the first to discover the → velocity-distance relation. Two years before Hubble, in 1927, Georges Lemaître (1894-1966) had derived the relation and published it in a paper in French which remained neglected (→ Friedmann-Lemaitre Universe). The International Astronomical Union (IAU) at its 30th Meeting approved the Resolution B4 proposed by the IAU Executive Committee recommending the use of Hubble-Lemaitre law instead of Hubble's law, after Edwin Hubble (1889-1953), the American astronomer who published his results in 1929 and Georges Lemaître, Belgian priest and astronomer, who published a paper on the expansion of the Universe in 1927; → law. |
Hubble-Lemaitre parameter pârânmun-e Hubble-Lemaître Fr.: paramètre de Hubble-Lemaître The rate pf change of the → cosmic scale factor: H(t) = (dR/dt)/R. The Hubble parameter is a time-dependent quantity and therefore is not constant. The → Hubble-Lemaitre constant is the Hubble-Lemaître parameter measured today. → Hubble-Lemaitre law; → parameter. |
Hubble-Lemaitre tension taneš-e pâyâ-ye Hubble-Lemaître Fr.: Tension sur la constante de Hubble-Lemaître The discrepancy between the value of the → Hubble-Lemaitre constant inferred from a ΛCDM fit (→ Lambda cold dark matter model) to the → cosmic microwave background (CMB) and local measurements. The Universe appears to be expanding much faster now than predicted even with our latest understanding of its initial conditions and contents. Based on the → Hubble Space Telescope observations, the Hubble-Lemaitre constant is very recently estimated to be 74.03 km s^{-1} Mpc^{-1}. This value indicates that the Universe is expanding at a rate about 9% faster than that implied by the → Planck satellite's observations of the → early Universe, which give a value for the Hubble constant of 67.4 km s^{-1} Mpc^{-1}. For discussion, see D'Arcy Kenworthy et al. (2019, ApJ 875, 145). |
Hubble-Sandage classification radebandi-ye Hubble-Sandage Fr.: classification de Hubble-Sandage Same as the → Hubble classification. → Hubble; → Hubble-Sandage variable; → sequence. |
Hubble-Sandage variable vartande-ye Hubble-Sandage Fr.: variable de Hubble-Sandage A type of highly luminous → blue supergiant star with variable light, first discovered in the M31 and M33 galaxies; also called → S Doradus stars. They are now believed to be part of the class of → Luminous Blue Variable stars. → Hubble; Allan Rex Sandage (1926-2010), American cosmologist. |
Huge Hole surâx-e kalân Fr.: Trou Géant A region of the Universe, nearly a billion light-years across, mostly devoid of stars, gas, other normal matter, and also → dark matter. Situated at about 6 billion light-years from us, in projection on the the constellation → Eridanus, it shows up as a particularly cold region in the map of the → cosmic microwave background (CMB) radiation. Observations made using the → Very Large Array (VLA) radio telescope show a relative absence of matter in that area. Huge, from M.E. huge, hoge, from O.F. ahuge, ahoge "enormous," from a variant of → ad- + hoge "height," → high; → hole. Surâx, → hole; kalân "great, large, bulky." |
<< < -he Haf hal har har He hea hel hel Her Her hid hig hip hom hor hot Hub Hug hur hyd hyd hyg hyp > >>