An Etymological Dictionary of Astronomy and Astrophysics

A → Wolf-Rayet star whose spectrum shows emission lines of carbon and strong emission lines of oxygen O VI 3811-34 Å. In theoretical models, a W-R star whose carbon abundance at surface is larger than nitrogen abundance and has the abundance ratio (C + O) / He > 1 (in number).

See also: W short for Wolf-Rayet star, O for → oxygen.

A → Wolf-Rayet star whose spectrum shows emission lines of carbon and strong emission lines of oxygen O VI 3811-34 Å. In theoretical models, a W-R star whose carbon abundance at surface is larger than nitrogen abundance and has the abundance ratio (C + O) / He > 1 (in number).

See also: W short for Wolf-Rayet star, O for → oxygen.

An oxygen-rich → Wolf-Rayet star whose spectrum shows the following emission line characteristics:
No O IV 3400 Å, strong O VI 3811-34 Å, O V 5572-98 Å about or stronger than C IV 5801-12 Å, no C III 5696 Å.

See also: W, from → Wolf-Rayet; O, from → oxygen; → star.

An oxygen-rich → Wolf-Rayet star whose spectrum shows the following emission line characteristics:
No O IV 3400 Å, strong O VI 3811-34 Å, O V 5572-98 Å about or stronger than C IV 5801-12 Å, no C III 5696 Å.

See also: W, from → Wolf-Rayet; O, from → oxygen; → star.

An oxygen-rich → Wolf-Rayet star whose spectrum shows the following emission line characteristics: No O IV 3400 Å, strong O VI 3811-34 Å, O V 5572-98 Å weaker than C IV 5801-12 Å, no C III 5696 Å.

See also: W, from → Wolf-Rayet; O, from → oxygen; → star.

An oxygen-rich → Wolf-Rayet star whose spectrum shows the following emission line characteristics: No O IV 3400 Å, strong O VI 3811-34 Å, O V 5572-98 Å weaker than C IV 5801-12 Å, no C III 5696 Å.

See also: W, from → Wolf-Rayet; O, from → oxygen; → star.

1a) To incline to one side and to the other alternately, as a wheel, top, or other rotating body when not properly balanced.

1b) To move unsteadily from side to side; vacillate; waver.

2. A wobbling movement (Dictionary.com).

Etymology (EN): Probably from Low Ger. wabbeln “to wobble;”
cognate with O.N. vafla “hover about, totter,” related to vafra “move unsteadily.”

Etymology (PE): Palâpel “wobbling, unsteady motion” in štiyâni dialect, variant in colloquial Persian pilipili, pelpel (pilipili raftan, pilipili xordan).

1a) To incline to one side and to the other alternately, as a wheel, top, or other rotating body when not properly balanced.

1b) To move unsteadily from side to side; vacillate; waver.

2. A wobbling movement (Dictionary.com).

Etymology (EN): Probably from Low Ger. wabbeln “to wobble;”
cognate with O.N. vafla “hover about, totter,” related to vafra “move unsteadily.”

Etymology (PE): Palâpel “wobbling, unsteady motion” in štiyâni dialect, variant in colloquial Persian pilipili, pelpel (pilipili raftan, pilipili xordan).

A 70-year period of unusually low → solar activity, from about 1280 to 1350. See also the → Maunder minimum.

See also: → Wolf number; → minimum.

A 70-year period of unusually low → solar activity, from about 1280 to 1350. See also the → Maunder minimum.

See also: → Wolf number; → minimum.

A number indicating the degree of → sunspot  → activity. Same as → sunspot number and → relative sunspot number.

See also: Named after Johann Rudolf Wolf of Zurich who introduced the number in 1852; → number.

A number indicating the degree of → sunspot  → activity. Same as → sunspot number and → relative sunspot number.

See also: Named after Johann Rudolf Wolf of Zurich who introduced the number in 1852; → number.

A → dwarf irregular galaxy that is a remote and rather isolated member of the → Local Group. Also known as DDO 221 and LEDA 143. It is a dim galaxy located in the constellation → Cetus, about three million → light-years from the → Milky Way. Its nearest neighbor, the → dwarf galaxy IC 1613, is one million light-years away. Quite elongated, with a largest extension of more than 8,000 light-years, WLM is about 12 times smaller than the Milky Way, a measurement that includes a → halo of extremely → old stars. WLM has a → metallicity only about one-tenth that of the Milky Way.

See also: Named after astronomer Max Wolf (1863-1932), who discovered the galaxy in 1909, and astronomers Knut Lundmark (1889-1958) and Philibert Jacques Melotte (1880-1961), who identified it as a galaxy some fifteen years later.

A → dwarf irregular galaxy that is a remote and rather isolated member of the → Local Group. Also known as DDO 221 and LEDA 143. It is a dim galaxy located in the constellation → Cetus, about three million → light-years from the → Milky Way. Its nearest neighbor, the → dwarf galaxy IC 1613, is one million light-years away. Quite elongated, with a largest extension of more than 8,000 light-years, WLM is about 12 times smaller than the Milky Way, a measurement that includes a → halo of extremely → old stars. WLM has a → metallicity only about one-tenth that of the Milky Way.

See also: Named after astronomer Max Wolf (1863-1932), who discovered the galaxy in 1909, and astronomers Knut Lundmark (1889-1958) and Philibert Jacques Melotte (1880-1961), who identified it as a galaxy some fifteen years later.

A subset of → starburst galaxies whose integrated spectra show broad emission features attributed to the presence of hundreds to thousands
→ Wolf-Rayet stars. The most massive stars formed in the burst evolve rapidly into a substantial population of Wolf-Rayet stars in aggregations of ionized gas.

See also: → Wolf-Rayet star; → galaxy.

A subset of → starburst galaxies whose integrated spectra show broad emission features attributed to the presence of hundreds to thousands
→ Wolf-Rayet stars. The most massive stars formed in the burst evolve rapidly into a substantial population of Wolf-Rayet stars in aggregations of ionized gas.

See also: → Wolf-Rayet star; → galaxy.

A type of very luminous, very hot (as high as 50,000 K) stars whose spectrum is characterized by broad emission lines (mainly He I and He II), which are presumed to originate from material ejected from the star at very high (~ 2000 km s^-1) velocities. The most massive → O stars (M > 25 → solar masses for → solar metallicity) become W-R stars around 2 and 3 million years after their birth, spending only some few hundreds of thousands of years (≤ 10⁶ years) in this phase until they explode as → type Ib and → type Ic supernovae. The minimum stellar mass that an O star needs to reach the W-R phase and its duration is dependent on → metallicity. → WC Wolf-Rayet; → WNE Wolf-Rayet; → WNL Wolf-Rayet; → WO Wolf-Rayet. For a review see: P. A. Crowther, 2007, Annu. Rev. of Astron. Astrophys. 45, 177.

See also: Named after the French astronomers Charles Wolf (1827-1918) and Georges Rayet (1839-1906), of the Paris Observatory.
In 1867 they discovered three stars in the constellation Cygnus (now designated HD191765, HD192103, and HD192641), that displayed broad emission bands in their spectra; → star.

A type of very luminous, very hot (as high as 50,000 K) stars whose spectrum is characterized by broad emission lines (mainly He I and He II), which are presumed to originate from material ejected from the star at very high (~ 2000 km s^-1) velocities. The most massive → O stars (M > 25 → solar masses for → solar metallicity) become W-R stars around 2 and 3 million years after their birth, spending only some few hundreds of thousands of years (≤ 10⁶ years) in this phase until they explode as → type Ib and → type Ic supernovae. The minimum stellar mass that an O star needs to reach the W-R phase and its duration is dependent on → metallicity. → WC Wolf-Rayet; → WNE Wolf-Rayet; → WNL Wolf-Rayet; → WO Wolf-Rayet. For a review see: P. A. Crowther, 2007, Annu. Rev. of Astron. Astrophys. 45, 177.

See also: Named after the French astronomers Charles Wolf (1827-1918) and Georges Rayet (1839-1906), of the Paris Observatory.
In 1867 they discovered three stars in the constellation Cygnus (now designated HD191765, HD192103, and HD192641), that displayed broad emission bands in their spectra; → star.

An optical device for producing and analyzing polarized light. It divides
incoming unpolarized light into two orthogonal, linearly polarized beams. It consists of two prisms of either quartz or calcite cemented together.

See also: After the English scientist William Hyde Wollaston (1766-1828); → prism.

An optical device for producing and analyzing polarized light. It divides
incoming unpolarized light into two orthogonal, linearly polarized beams. It consists of two prisms of either quartz or calcite cemented together.

See also: After the English scientist William Hyde Wollaston (1766-1828); → prism.

A → grazing incidence telescope designed to observe → X-ray emission from astronomical objects. Wolter telescopes use a combination of two elements, a parabolic mirror followed by a hyperbolic mirror and come in three different optical configurations.

The design most commonly used by X-ray astronomers is the Type I since it has the simplest mechanical configuration. In addition, the Type I design offers the possibility of nesting several telescopes inside one another, thereby increasing the useful reflecting area. This is an extremely important attribute, since virtually all X-ray sources are weak, and maximizing the light-gathering power of a mirror system is critical. The → Chandra X-Ray Observatory is a Wolter Type I telescope that has four thick nested mirrors coated in iridium. The Japanese X-ray observatory Suzuki uses a conical approximation of the Wolter Type I design. Its mirrors are coated in gold, and they are far thinner than the ones used in Chandra. This allows for denser nesting, so there are 700 mirrors instead of four. The result is a much higher collecting efficiency at a reduced weight.

For comparable apertures and grazing angles, the primary advantage of Type II over Type I is that higher magnifications are attainable. This is because the second reflection is off the outside of a surface, which allows longer focal lengths. However, since off-axis images suffer much more severely from blurring in Type II configurations, the Wolter Type II is useful only as a narrow-field imager or as the optic for a dispersive spectrometer. The Wolter Type III has never been employed for X-ray astronomy (NASA Imagine the Universe!).

See also: Named after Hans Wolter (1911-1978), a German physicist who designed the optical configuration.

A → grazing incidence telescope designed to observe → X-ray emission from astronomical objects. Wolter telescopes use a combination of two elements, a parabolic mirror followed by a hyperbolic mirror and come in three different optical configurations.

The design most commonly used by X-ray astronomers is the Type I since it has the simplest mechanical configuration. In addition, the Type I design offers the possibility of nesting several telescopes inside one another, thereby increasing the useful reflecting area. This is an extremely important attribute, since virtually all X-ray sources are weak, and maximizing the light-gathering power of a mirror system is critical. The → Chandra X-Ray Observatory is a Wolter Type I telescope that has four thick nested mirrors coated in iridium. The Japanese X-ray observatory Suzuki uses a conical approximation of the Wolter Type I design. Its mirrors are coated in gold, and they are far thinner than the ones used in Chandra. This allows for denser nesting, so there are 700 mirrors instead of four. The result is a much higher collecting efficiency at a reduced weight.

For comparable apertures and grazing angles, the primary advantage of Type II over Type I is that higher magnifications are attainable. This is because the second reflection is off the outside of a surface, which allows longer focal lengths. However, since off-axis images suffer much more severely from blurring in Type II configurations, the Wolter Type II is useful only as a narrow-field imager or as the optic for a dispersive spectrometer. The Wolter Type III has never been employed for X-ray astronomy (NASA Imagine the Universe!).

See also: Named after Hans Wolter (1911-1978), a German physicist who designed the optical configuration.

In → magnetohydrodynamics, in the limit of zero → resistivity, the → magnetic field  B satisfies the → induction equation  ∂B/∂t = ∇ x (v x B), then for a → plasma confined by a perfectly conducting boundary, the → magnetic helicity is conserved. If the normal field is fixed on the boundary, the minimum-energy state is the linear → force-free magnetic field that conserves the total magnetic helicity.

See also: Named after the Dutch astrophysicist Lodewijk Woltjer (1930-2019), who discovered the phenomenon in 1958 while studying the → Crab Nebula; → theorem.

In → magnetohydrodynamics, in the limit of zero → resistivity, the → magnetic field  B satisfies the → induction equation  ∂B/∂t = ∇ x (v x B), then for a → plasma confined by a perfectly conducting boundary, the → magnetic helicity is conserved. If the normal field is fixed on the boundary, the minimum-energy state is the linear → force-free magnetic field that conserves the total magnetic helicity.

See also: Named after the Dutch astrophysicist Lodewijk Woltjer (1930-2019), who discovered the phenomenon in 1958 while studying the → Crab Nebula; → theorem.

The → female human being.

Etymology (EN): M.E. womman, wimman, O.E. wifman, from wif “female” + man “human being.”

Etymology (PE): Zan “woman, wife” (variants Baluci, Zâzâ jan, Gorgâni cen, Baxtiyâri zine, Sangesari, Tâti, Kurd. žen, Kurd. kenâ, Karingâni yan); Mid.Pers. zan “woman, wife;” kaniz “maid, virgin, girl;” Av. jəni- “woman, wife;” cf. Skt. jáni- “woman, wife;” Gk. gyne “woman, wife;” O.E. cwen “queen, woman, wife” (E. queen; Arm. kin “woman;” PIE base *g^wenh- “woman, wife.”

The → female human being.

Etymology (EN): M.E. womman, wimman, O.E. wifman, from wif “female” + man “human being.”

Etymology (PE): Zan “woman, wife” (variants Baluci, Zâzâ jan, Gorgâni cen, Baxtiyâri zine, Sangesari, Tâti, Kurd. žen, Kurd. kenâ, Karingâni yan); Mid.Pers. zan “woman, wife;” kaniz “maid, virgin, girl;” Av. jəni- “woman, wife;” cf. Skt. jáni- “woman, wife;” Gk. gyne “woman, wife;” O.E. cwen “queen, woman, wife” (E. queen; Arm. kin “woman;” PIE base *g^wenh- “woman, wife.”

A unit of language, consisting of one or more sounds or their written representation, that communicates a meaning. → stopword

Etymology (EN): M.E., from O.E. word; cf. Du. woord, O.H.G., Ger. wort, Goth. waurd; related to verb, from L. verbum “verb;” from PIE *wer- “to speak, say.”

Etymology (PE): Vâžé “word;” Mid.Pers. vâc, vâcak “word, speech;” related to âva “voice, sound,” âvâz “voice, sound, song,” bâng “voice, sound, clamour” (Mid.Pers. vâng); Av. vacah- “word,” vaocanghê “to decalre” (by means of speech), from vac- “to speak, say;” cf. Skt. vakti “speaks, says,” vacas- “word;”
Gk. epos “word;” L. vox “voice;” PIE base *wek- “to speak.”

A unit of language, consisting of one or more sounds or their written representation, that communicates a meaning. → stopword

Etymology (EN): M.E., from O.E. word; cf. Du. woord, O.H.G., Ger. wort, Goth. waurd; related to verb, from L. verbum “verb;” from PIE *wer- “to speak, say.”

Etymology (PE): Vâžé “word;” Mid.Pers. vâc, vâcak “word, speech;” related to âva “voice, sound,” âvâz “voice, sound, song,” bâng “voice, sound, clamour” (Mid.Pers. vâng); Av. vacah- “word,” vaocanghê “to decalre” (by means of speech), from vac- “to speak, say;” cf. Skt. vakti “speaks, says,” vacas- “word;”
Gk. epos “word;” L. vox “voice;” PIE base *wek- “to speak.”

If a force F acting on a body moves its point of application through a distance r, the work is defined by the product F.r.cosθ, where θ is the angle between the line of action of the force and the displacement. Work can be positive, negative, or zero.

Etymology (EN): M.E.; O.E. weorc, worc “something done, action, military fortification,” from P.Gmc. *werkan (cf. O.S., O.Fris., Du. werk, O.N. verk, O.H.G. werah, Ger. Werk), from PIE base *werg- “to work;” cognate with Pers. varz-, varzidan “to labor, practise,” → erg.

Etymology (PE): Kâr “work,” Mid.Pers kâr; Mod./Mid.Pers. kardan “to do, to work,” Mid.Pers. kardan; O.Pers./Av. kar- “to do, make, build,” Av. kərənaoiti “he makes;” cf. Skt. kr- “to do, to make,” krnoti “he makes, he does,”
karoti “he makes, he does,” karma “act, deed;” PIE base k^wer- “to do, to make.”

If a force F acting on a body moves its point of application through a distance r, the work is defined by the product F.r.cosθ, where θ is the angle between the line of action of the force and the displacement. Work can be positive, negative, or zero.

Etymology (EN): M.E.; O.E. weorc, worc “something done, action, military fortification,” from P.Gmc. *werkan (cf. O.S., O.Fris., Du. werk, O.N. verk, O.H.G. werah, Ger. Werk), from PIE base *werg- “to work;” cognate with Pers. varz-, varzidan “to labor, practise,” → erg.

Etymology (PE): Kâr “work,” Mid.Pers kâr; Mod./Mid.Pers. kardan “to do, to work,” Mid.Pers. kardan; O.Pers./Av. kar- “to do, make, build,” Av. kərənaoiti “he makes;” cf. Skt. kr- “to do, to make,” krnoti “he makes, he does,”
karoti “he makes, he does,” karma “act, deed;” PIE base k^wer- “to do, to make.”

The least amount of energy required to remove an electron from the surface of a solid, to a point just outside the solid where the electron has zero kinetic energy. See also → photoelectric effect.

See also: → work; → function.

The least amount of energy required to remove an electron from the surface of a solid, to a point just outside the solid where the electron has zero kinetic energy. See also → photoelectric effect.

See also: → work; → function.

The → work of the resultant force exerted on a particle equals the change in kinetic energy of the particle.

See also: → work; → energy; → principle.

The → work of the resultant force exerted on a particle equals the change in kinetic energy of the particle.

See also: → work; → energy; → principle.

A group of people working together to achieve a stated goal.

See also: → work; → -ing; → group.

A group of people working together to achieve a stated goal.

See also: → work; → -ing; → group.

The double shock structure formed in any two fluids that collide supersonically. A working surface consists of two → shocks, a → bow shock where the ambient material is shocked and accelerated, and a jet shock or → Mach disk, where the → jet material is decelerated. It is common to find multiple working surfaces along the axis of an → Herbig-Haro jet, testifying to recurrent eruptions of the underlying source.

See also: → work; → -ing; → surface.

The double shock structure formed in any two fluids that collide supersonically. A working surface consists of two → shocks, a → bow shock where the ambient material is shocked and accelerated, and a jet shock or → Mach disk, where the → jet material is decelerated. It is common to find multiple working surfaces along the axis of an → Herbig-Haro jet, testifying to recurrent eruptions of the underlying source.

See also: → work; → -ing; → surface.

1. A place where manual work is done, especially manufacturing or repairing.
   

2. A group of people working on a creative project, discussing a topic, or studying a subject.

Etymology (EN): → work + shop M.E. shoppe, O.E. sceoppa;
cf. O.H.G. scopf “porch,” Ger. Schuppen “a shed”).

Etymology (PE): Kârgâh “workshop,” from kâr, → work, + gâh “place; time” (Mid.Pers. gâh, gâs “time;” O.Pers. gāθu-; Av. gātav-, gātu- “place, throne, spot;” cf. Skt. gâtu- “going, motion; free space for moving; place of abode;” PIE *gwem- “to go, come”).

1. A place where manual work is done, especially manufacturing or repairing.
   

2. A group of people working on a creative project, discussing a topic, or studying a subject.

Etymology (EN): → work + shop M.E. shoppe, O.E. sceoppa;
cf. O.H.G. scopf “porch,” Ger. Schuppen “a shed”).

Etymology (PE): Kârgâh “workshop,” from kâr, → work, + gâh “place; time” (Mid.Pers. gâh, gâs “time;” O.Pers. gāθu-; Av. gātav-, gātu- “place, throne, spot;” cf. Skt. gâtu- “going, motion; free space for moving; place of abode;” PIE *gwem- “to go, come”).

1. The Earth with its inhabitants. Compare → cosmos and → Universe.
   

2. Other planets, particularly → exoplanets.
   

3. Any realm, or domain, with all pertaining to it.
   

4. Physics: The → space-time in four dimensions, as distinguished from three-dimensional space. → world line.

Etymology (EN): M.E.; O.E. woruld, weorold; cf. O.S. werold, O.Fris. warld, Du. wereld, O.N. verold, O.H.G. weralt, Ger. Welt.

Etymology (PE): Jahân, variants keyhân, geyhân “world,” giti “world, material world, time;” Mid.Pers. gêhân “world,” gêtig “the material world; wordly,” Manichean Mid.Pers. gyh “world,” gyh’n “worlds;” Av. gaēθā- “being, world, matter, mankind” (O.Pers. gaiθā- “livestock”), gaya- “life, manner of living,” root gay- “to live” (present tense jiva-), cognate with Skt. jīv- “to live,” jīva- “alive, living;” Gk. bios “life,” L. vivus “living, alive,” vita “life;” PIE base *g^wei- “to live” (cf. O.E. cwic “alive;” O.C.S. zivo “to live;” Lith. gyvas “living, alive;” O.Ir. bethu “life,” bith “age, life, world;” Welsh byd “world”). The Pers. words zistan “to live,” zendé “alive,” zendegi “life,” and jân “vital spirit, soul; mind” belong to this family.

1. The Earth with its inhabitants. Compare → cosmos and → Universe.
   

2. Other planets, particularly → exoplanets.
   

3. Any realm, or domain, with all pertaining to it.
   

4. Physics: The → space-time in four dimensions, as distinguished from three-dimensional space. → world line.

Etymology (EN): M.E.; O.E. woruld, weorold; cf. O.S. werold, O.Fris. warld, Du. wereld, O.N. verold, O.H.G. weralt, Ger. Welt.

Etymology (PE): Jahân, variants keyhân, geyhân “world,” giti “world, material world, time;” Mid.Pers. gêhân “world,” gêtig “the material world; wordly,” Manichean Mid.Pers. gyh “world,” gyh’n “worlds;” Av. gaēθā- “being, world, matter, mankind” (O.Pers. gaiθā- “livestock”), gaya- “life, manner of living,” root gay- “to live” (present tense jiva-), cognate with Skt. jīv- “to live,” jīva- “alive, living;” Gk. bios “life,” L. vivus “living, alive,” vita “life;” PIE base *g^wei- “to live” (cf. O.E. cwic “alive;” O.C.S. zivo “to live;” Lith. gyvas “living, alive;” O.Ir. bethu “life,” bith “age, life, world;” Welsh byd “world”). The Pers. words zistan “to live,” zendé “alive,” zendegi “life,” and jân “vital spirit, soul; mind” belong to this family.

In relativity, the path traced out in four-dimensional → space-time that represents a continuous sequence of events relating to a given particle. A point on a world line is called an → event. Any straight world line corresponds to an → inertial motion. Curved world lines represent → accelerated motion. A world line that curves corresponds to an accelerated observer. World lines are shown on space-time diagrams.

See also: → world; → line.

In relativity, the path traced out in four-dimensional → space-time that represents a continuous sequence of events relating to a given particle. A point on a world line is called an → event. Any straight world line corresponds to an → inertial motion. Curved world lines represent → accelerated motion. A world line that curves corresponds to an accelerated observer. World lines are shown on space-time diagrams.

See also: → world; → line.

A hypothetical topological feature, based on → general relativity, that connects two different points like a “tunnel” in → space-time.
The most common concept of a wormhole is an → Einstein-Rosen bridge. A trip through the wormhole could take much less time than a journey between the same starting and ending points in normal space. Wormholes have various types, intra-universe wormholes (connecting two distant regions of our Universe with each other) and inter-universe wormholes (that connect our Universe with another universe).

Etymology (EN): The term was coined by the Princeton physicist John Wheeler (1911-2008), from worm, M.E., O.E. wurm “serpent, dragon;” cf. O.S., O.H.G., Ger. wurm, O.Fris., Du. worm, Goth. waurms “serpent, worm;” akin to Pers. kerm “worm,” as below; → hole.

Etymology (PE): Kerm “worm;” Mid.Pers. kirm “worm, snake, dragon;” cf. Skt. krmi- “worm, maggot;” O.Ir. cruim “worm;” Lith. kirmis “worm;” L. vermis “worm;” E. worm, as above; surâx,
→ hole.

A hypothetical topological feature, based on → general relativity, that connects two different points like a “tunnel” in → space-time.
The most common concept of a wormhole is an → Einstein-Rosen bridge. A trip through the wormhole could take much less time than a journey between the same starting and ending points in normal space. Wormholes have various types, intra-universe wormholes (connecting two distant regions of our Universe with each other) and inter-universe wormholes (that connect our Universe with another universe).

Etymology (EN): The term was coined by the Princeton physicist John Wheeler (1911-2008), from worm, M.E., O.E. wurm “serpent, dragon;” cf. O.S., O.H.G., Ger. wurm, O.Fris., Du. worm, Goth. waurms “serpent, worm;” akin to Pers. kerm “worm,” as below; → hole.

Etymology (PE): Kerm “worm;” Mid.Pers. kirm “worm, snake, dragon;” cf. Skt. krmi- “worm, maggot;” O.Ir. cruim “worm;” Lith. kirmis “worm;” L. vermis “worm;” E. worm, as above; surâx,
→ hole.