An Etymological Dictionary of Astronomy and Astrophysics
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فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory

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Hubble Deep Field (HDF)
  میدان ِ ژرف ِ هابل   
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; → deep; → field.

Hubble diagram
  نمودار ِ هابل   
nemudâr-e Hubble (#)

Fr.: diagramme de Hubble   

A plot of the → redshift of galaxies against their distance or against their → apparent magnitude.

Hubble; → diagram.

Hubble distance
  دورای ِ هابل   
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; → distance.

Hubble flow
  تچان ِ هابل   
tacân-e Hubble

Fr.: flot de Hubble   

Hubble-Lemaitre flow.

Hubble; → flow.

Hubble law
  قانون ِ هابل   
qânun-e Hubble

Fr.: loi de Hubble   

Hubble-Lemaitre law.

Hubble; → law.

Hubble length
  درازای ِ هابل   
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; → length.

Hubble parameter
  پارامون ِ هابل   
pârânmun-e Hubble

Fr.: paramètre de Hubble   

Hubble-Lemaitre parameter.

Hubble; → parameter.

Hubble radius
  شعاع ِ هابل   
šo'â'-e Hubble (#)

Fr.: rayon de Hubble   

The size of the observable Universe as derived from the ratio c/H0, where H0 is the → Hubble-Lemaitre constant and c the → speed of light. Same as → Hubble distance, → Hubble length, and → cosmic horizon.

Hubble; → radius.

Hubble sequence
  پی‌آیه‌ی ِ هابل   
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; → sequence.

Hubble Space Telescope (HST)
  دوربین ِ فضایی ِ هابل، تلسکوپ ِ ~ ~   
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; → space; → telescope.

Hubble time
  زمان ِ هابل   
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: tH = 1/H0. Also called the Hubble age or the Hubble period.

Hubble; → time.

Hubble-Lemaitre constant
  پایا‌ی ِ هابل-لومتر   
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 H0 = 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
  تچان ِ هابل-لومتر   
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
  قانون ِ هابل-لومتر   
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 = H0d, where v is the recessional velocity, H0 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
  پارامون ِ هابل-لومتر   
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
  تنش ِ پایای ِ هابل-لومتر   
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-Lamaitre constant; → tension.

Hubble-Sandage classification
  رده‌بندی ِ هابل-سندیج   
radebandi-ye Hubble-Sandage

Fr.: classification de Hubble-Sandage   

Same as the → Hubble classification.

Hubble; → Hubble-Sandage variable; → sequence.

Hubble-Sandage variable
  ورتنده‌ی ِ هابل-سندیج   
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
  سوراخ ِ کلان   
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."

Huggins band
  باند ِ هاگینس   
bând-e Huggins

Fr.: bande de Huggins   

A band in the → absorption spectrum of → ozone (O3) extending in the → ultraviolet from 310 nm to 370 nm. It is located at the red end of the strong → Hartley band.

W. Huggins and M. Huggins, Proc. R. Soc. London 48, 216 (1890).

<< < -es -it -sc 201 951 abe abs abs aca acc acc aco act ada adh ado aer aft air Alf alg alk alp Alt alt amb ana And ang ani ann ant ant ant apo app app Apu arc arg Arn art ass ast ast ast atm ato att aur aut avo azi bac bal bar bar bat Bea Bel bet bia big bin bio Bir bla bla blo Blu bol Boo bou box bre Bri bro bur cal cal Can cap car Car cat cau cel cen cen cha Cha cha che Chi chr cir cir civ cla clo clo CMB coa coe coh col col col com com com com com com com com Com con con con con con con con con con con con con coo cor cor cor Cos cos cos cou cou cra cri cro cry cul cur cyc D l dar dat day dea dec dec dec def def deg Del Den dep der det deu dew dic dif dif dil dip dir dis dis dis dis dis diu dog Dop dou Dra Dsc dus dwa dyn Dys Ear ecc eco edg egg Ein Ela ele ele ele ele ell eme emp enc eng ent epi equ equ equ eru eth Eur eve exa exc exe exi exo exp ext ext ext fab fai Fan fea fem fer fie fil fir fir fla fli flu foc for for for fra fre fre fri fun fuz gal gal gal Gam gau Gau gen geo geo geo geo Gib glo gov gra gra gra gra gre gro Gui H-a hal Ham har Hay hea hei hel Hel her het hie hig hoa hom hor hot Hub Hug hur hyd hyd hyl hyp ice ide ima ima imp imp inc inc ind ine inf inf inf ing inn ins ins int int int int int int int int inv inv ion iro Isl iso iso Jab jet Jov Jup Kar Kep kil Kip Kra Lag Lam Lan Lar las law lea Leg Leo lev lig lim lin lin lin lit loc loc log Lor low lum lun lun Lym Mac mag mag mag mag mag mai Mal map mas mas mat Mau mea mea med Men mer Mes Met met mic mic Mie mil min Mir mix mod mol mom Moo mor mov mul mur n-b nan nat nea neg Ner neu new New NGC noc nom non non nor nor nuc nuc nul nut obj obl obs occ oct off old one ope opp opt opt orb ord org Ori osc oth ove Owl P-s Pal par par par par Pas pat pec pen per per per per per Pha pha pho pho pho phy pie pix Pla pla pla pla Pli Poi pol pol pol pol por pos pos pow pre pre pre pre pri pri pri pro pro pro pro pro pro pro pub pul pyc qua qua qua qua qui rad rad rad rad rad rad rai ran rar Ray rea Rea rec rec red red ref ref reg rel rel rel ren res res res res ret rev Ric rig rin roc roo rot rot rur S5- Sal sat sca sca Sch sci Scu sec sec sed sel sel sem seq set sha she sho sid sie sil sim sin sit sky slo sno sod sol sol sol sol son sou spa spa spe spe spe spe sph spi spo squ sta sta sta sta ste ste ste Sti sto str str sub sub sub sul sup sup sup sup sur sur syl syn sys tal Tay tel ten ter tex the the the the Tho thr tid tim Tit too Tor tra tra Tra tra Tra tri Tri tru tub tur two Typ ult ult unc uni uni uni upl ura uti val var vec vel ver Ver vie vir vis vis vol W-R war wav wav wea Wei wha wid win WN3 Wol wri xen yok zen zij > >>