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Region of an astronomical diagram
The unqualified term instability strip usually refers to a region of the Hertzsprung–Russell diagram largely occupied by several related classes of pulsating
Instability_strip
Scatter plot of stars showing the relationship of luminosity to stellar classification
in a section of the diagram called the instability strip. Cepheid variables also fall on the instability strip, at higher luminosities. The H-R diagram
Hertzsprung–Russell_diagram
Stars with a supergiant luminosity class with a spectral type of K or M
stars are the RV Tauri variables, AGB or post-AGB stars lying on the instability strip and showing distinctive semi-regular variations. Red supergiants develop
Red_supergiant
Continuous band of stars that appears on plots of stellar color versus brightness
composition. A nearly vertical region of the HR diagram, known as the instability strip, is occupied by pulsating variable stars known as Cepheid variables
Main_sequence
Stage of stellar evolution
cross the instability strip during a blue loop are thought to become W Virginis variables. More massive stars, crossing the instability strip during a
Blue_loop
Northern pole-star; brightest star in Ursa Minor
thought to be due to secular redward evolution across the Cepheid instability strip, but it may be due to interference between the primary and the first-overtone
Polaris
Star whose brightness fluctuates, as seen from Earth
diagram. They occupy a separate LBV/S Dor instability strip, which is distinct from the Cepheid instability strip. Yellow hypergiants These massive evolved
Variable_star
Class of massive star with a spectral type of A to K
hypergiants occupy a region of the Hertzsprung–Russell diagram above the instability strip, a region where relatively few stars are found and where those stars
Yellow_hypergiant
Type of star, larger and brighter than the Sun
unstable, leading to the instability strip on the HR diagram where the majority of stars are pulsating variables. The instability strip reaches from the main
Giant_star
Type of variable star
star (IMS) first evolves away from the main sequence, it crosses the instability strip rapidly while the hydrogen shell is still burning. When the helium
Classical_Cepheid_variable
Distant star or star cluster
Upper portion of H-R Diagram showing the location of the S Doradus instability strip and the location of LBV outbursts. Main sequence is the thin sloping
WHL0137-LS
Type of star larger than main-sequence but smaller than a giant
massive than the sun cross the Cepheid instability strip, called the first crossing since they may cross the strip again later on a blue loop. In the 2
Subgiant
Changes to stars over their lifespans
temperatures, some becoming unstable pulsating stars in the yellow instability strip (RR Lyrae variables), whereas some become even hotter and can form
Stellar_evolution
Stellar core remnant
O'Brien, M. S. (2000). "The Extent and Cause of the Pre–White Dwarf Instability Strip". The Astrophysical Journal. 532 (2): 1078–1088. arXiv:astro-ph/9910495
White_dwarf
Type of variable star that pulsates radially
the instability strip and were originally referred to as dwarf Cepheids. RR Lyrae variables have short periods and lie on the instability strip where
Cepheid_variable
Type of variable star
known periods range between 5 and 23 minutes. They lie in the δ Scuti instability strip on the main sequence. The first roAp star to be discovered was HD
Rapidly_oscillating_Ap_star
Rare star with tremendous luminosity and high rates of mass loss by stellar winds
luminosity over time due to instabilities within their interiors, but these are small except for two distinct instability regions where luminous blue
Hypergiant
Theoretical stellar remnant
or metals Chthonian planet – Gas giants with their atmospheric layers stripped Heger, A.; Fryer, C. L.; et al. (2003). "How Massive Single Stars End Their
Black_dwarf
Light from the stars
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Starlight
Star that has a supergiant luminosity class, with a spectral type of F or G
yellow supergiants are in a region of the HR diagram known as the instability strip because their temperatures and luminosities cause them to be dynamically
Yellow_supergiant
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Lists of stars by constellation
Lists_of_stars_by_constellation
Stage of stellar evolution
cluster has no stars in this region of its CMD. The gap occurs at the instability strip, where many pulsating stars are found. These pulsating horizontal-branch
Horizontal_branch
Type of star that is luminous, blue, and variable in brightness
region of the Hertzsprung–Russell diagram known as the S Doradus instability strip, where the least luminous have a temperature around 10,000 K and a
Luminous_blue_variable
Type of star that is massive and luminous
types of variables amongst the supergiants are well defined. The instability strip crosses the region of supergiants, and specifically many yellow supergiants
Supergiant
Portion of the giant branch before helium ignition
more at luminosities of thousands of L☉. These stars will cross the instability strip more than once and pulsate as Type I (Classical) Cepheid variables
Red-giant_branch
Type of neutron star with beams of radiation
terrestrial source. On November 28, 1967, Bell and Hewish using a fast strip chart recorder resolved the signals as a series of pulses, evenly spaced
Pulsar
Hypothesized alternative to a black hole
Paolo; Cadoni, Mariano; Cavaglià, Marco (26 June 2008). "Ergoregion instability of ultracompact astrophysical objects". Physical Review D. 77 (12) 124044
Gravastar
Stellar classification
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
G-type_main-sequence_star
Type of neutron star with a strong magnetic field
result from the death of very large stars as pair-instability supernovae (or pulsational pair-instability supernovae). However, recent research by astronomers
Magnetar
Star in the Large Magellanic Cloud
lie along a diagonal band in the H–R diagram called the S Doradus Instability Strip, with the more luminous examples having hotter temperatures. The standard
S_Doradus
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
List_of_brightest_stars
Natural physical entity in space
can cause it to become a variable star. An example of this is the instability strip, a region of the H-R diagram that includes Delta Scuti, RR Lyrae and
Astronomical_object
Type of large cool star
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Red_giant
Hypothetical compact star
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Q_star
Non-orientable surface with one edge
Raymond E.; Alexander, Gareth P.; Moffatt, H. Keith (2015). "Instability of a Möbius strip minimal surface and a link with systolic geometry" (PDF). Physical
Möbius_strip
Structure formed by diffuse material in orbital motion around a massive central body
uneven irradiance, magnetohydrodynamic effects, and other forces induce instabilities causing orbiting material in the disk to spiral inward toward the central
Accretion_disk
Stellar classification
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
K-type_main-sequence_star
Star's outer shell from which light is radiated
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Photosphere
Astronomical category of stars
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Iron_star
Early stage in the process of star formation
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Protostar
Astrophysical phenomenon
mechanisms: exceeding the Chandrasekhar limit; electron capture; pair-instability; or photodisintegration. When a massive star develops an iron core larger
Supernova
Subdwarf star with spectral type B
short-period pulsators cluster together in the so-called empirical instability strip, approximately defined by T=28,000–35,000 K (27,700–34,700 °C; 49
Subdwarf_B_star
Outermost layer of a star's atmosphere
stellar envelopes emit this radiation during shocks due to thermal instabilities in rapidly moving gas blobs. Also A-stars do not have convection zones
Stellar_corona
Chemically peculiar stars of spectral types A and B
(Przybylski's star). These stars lie at the bottom of the Delta Scuti instability strip, on the main sequence. There are currently 35 known roAp stars. The
Ap_and_Bp_stars
Hypothetical class of star that develops from a red dwarf
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Blue_dwarf_(red-dwarf_stage)
Hypothetical early-universe star with a black hole core
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Quasi-star
Gas and dust surrounding a newly formed star
outer space that creates a dead zone in which the magnetorotational instability (MRI) no longer operates. It is believed that these disks consist of
Protoplanetary_disk
Hypothetical hybrid star type
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Thorne–Żytkow_object
B-type star with emission lines
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Be_star
Star at the centre of the Solar System
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Sun
Creation of chemical elements within stars
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Stellar_nucleosynthesis
Small number of stars that orbit each other
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Star_system
Dim, low mass stars on the main sequence
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Red_dwarf
Star of relatively small size and low luminosity
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Dwarf_star
Event wherein the Sun is obscured by the Moon
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Solar_eclipse
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
List_of_nearest_stars
Study of oscillations in stars
effect. Delta Scuti variables are found roughly where the classical instability strip intersects the main sequence. They are typically A- to early F-type
Asteroseismology
Hypothetical star heated by dark-matter annihilation
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Dark_star_(dark_matter)
Central region of the Sun
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Solar_core
Class of astronomical objects
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Symbiotic_binary
Brightness of a celestial object observed from the Earth
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Apparent_magnitude
White dwarf whose luminosity is variable
dwarf binary system with a carbon-oxygen accretion disk. G 117-B15A Instability strip Stellar pulsation Koester & Chanmugam 1990, p. 891–895. Murdin, Paul
Pulsating_white_dwarf
Light emitted by the Sun
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Sunlight
Binary star system in the constellation Draco
strength of −1.16±0.25 G. Beta Draconis lies on or near the cepheid instability strip, yet only appears to be a microvariable with a range of about 1/100
Beta_Draconis
Type of star
studies predict these objects would be stable, while others predict instability. A survey examined the mass–radius relation for 40,000 white dwarfs and
Strange_star
Pattern of stars recognized on Earth's night sky
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Asterism_(astronomy)
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
List_of_proper_names_of_stars
Supernova that ejects a large mass at unusually high velocity
used to describe a theoretical type of supernova now known as a pair-instability supernova. It referred to the extremely high energy of the explosion
Hypernova
Isolated, small, and opaque nebula
that are irradiated by ultraviolet light from hot nearby stars exhibit stripping of materials to produce a tail. These types are called "cometary globules"
Bok_globule
Grouping of stars by similar metallicity
exhausted their fuel and likely exploded in extremely energetic pair-instability supernovae. Those explosions would have thoroughly dispersed their material
Stellar_population
Astronomical objects of planetary size that did not form in orbit around a star
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Sub-brown_dwarf
Hypothetical astronomical object
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Planck_star
Flow of gas ejected from the upper atmosphere of a star
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Stellar_wind
Collapsed core of a massive star
or the result of a second round of planet formation. Pulsars can also strip the atmosphere off from a star, leaving a planetary-mass remnant, which
Neutron_star
Hypothetical gravitational object composed of matter
same as a black star of equivalent mass and radius with the overlayment stripped off. Temperatures increase with depth towards the center. Black hole Dark-energy
Black star (semiclassical gravity)
Black_star_(semiclassical_gravity)
Classification in astronomy
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Compact_object
Unit of time
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Galactic_year
Stellar classification
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
F-type_main-sequence_star
List of the hottest known stars
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
List_of_hottest_stars
Hypothetical object that potentially explains accelerating universal expansion
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Dark-energy_star
Stellar classification distinguished by bright blue luminosity
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
B-type_main-sequence_star
ISSN 0035-8711. Glatzel, Wolfgang; Kraus, Michaela (23 March 2024). "Instabilities in the yellow hypergiant domain". Monthly Notices of the Royal Astronomical
List_of_largest_stars
Star in the constellation Crux
effective temperature of about 27,000 K it is at the hot edge of the instability strip where such stars are found. It has three different pulsation modes
Mimosa_(star)
Constellation in the northern celestial hemisphere
whose members can be found both inside and outside the Delta Scuti instability strip. Lambda Boötis stars are dwarf stars that can be either spectral class
Boötes
Outer region of the volume of a star
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Stellar_atmosphere
Star types predicted by theory
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Hypothetical_star
Variable star in the constellation Puppis
varies between F9 and G7 as its temperature changes. It lies on the instability strip and based on the rate of change of its period is thought to be crossing
RS_Puppis
Hot, giant star of early spectral type
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Blue_giant
Astronomical object without the mass to sustain hydrogen fusion
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Substellar_object
Hypothetical types of stars
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Exotic_star
Main-sequence star of spectral type O
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
O-type_main-sequence_star
Compact exotic star which forms matter consisting mostly of quarks
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Quark_star
Star that never sets due to its apparent proximity to a celestial pole
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Circumpolar_star
Stellar system in the constellation Carina
luminosity. LBVs in the quiescent state lie on a narrow S Doradus instability strip, with more luminous stars being hotter. In outburst all LBVs have
Eta_Carinae
Brightest star in the constellation of Carina
overlap during the blue loops. Canopus lies on the warm side of the instability strip and does not pulsate like Cepheid variables of a similar luminosity
Canopus
Calculated property of a star or planet
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Effective_temperature
Star in the constellation Pegasus
narrow, nearly vertical band of the HR diagram that is known as the instability strip. Stars in this band oscillate in a coherent manner, resulting in periodic
IK_Pegasi
Class of young variable stars
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
T_Tauri_star
Planetary system consisting of the Sun and objects orbiting it
caused each to migrate into different orbits. This led to dynamical instability of the entire system, which scattered the planetesimals and ultimately
Solar_System
Coming together of two stars
Planetary nebula Protoplanetary Wolf–Rayet nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Stellar population Supernova Superluminous
Stellar_collision
INSTABILITY STRIP
INSTABILITY STRIP
Surname or Lastname
English
English : nickname from Middle English stripling ‘youth’.
Surname or Lastname
English
English : occupational name for a worker in wood or a nickname for a thin person, from an agent derivative of Middle English latt ‘thin narrow strip of wood’, ‘lath’ (Old English lætt).Jewish (eastern Ashkenazic) : occupational name for a cobbler, tinker, or the like, from an agent derivative of Yiddish laten ‘to patch’, ‘to repair’.
Boy/Male
Arabic, Muslim
Firmness; Stability; Certainty; Endurance; Boldness; Truth
Girl/Female
Indian, Marathi
Stability; Discipline; Dedication; Over-cautious; Stubborn.
Girl/Female
Arabic, Muslim
Stability; Firmness; Certainty; Boldness; Truth; Endurance
Surname or Lastname
English
English : variant spelling of Ling 1.Norwegian : habitational name from any of several farmsteads in western Norway named with lyng ‘heather’, either on its own, or with the addition of vin ‘meadow’.Dutch (de Linge) and North German : habitational name from a place named with Old Low German linge ‘strip of land or water’, or possibly with the river name Linge (this river flows through the Betuwe). See also Lingen.Possibly French, from a metonymic occupational name from linge ‘linen goods’, but there is no evidence of surname in North America.
Surname or Lastname
English and Irish
English and Irish : apparently a topographic name from Middle English furlong ‘length of a field’ (from Old English furh ‘furrow’ + lang ‘long’), the technical term for the block of strips owned by several different persons which formed the unit of cultivation in the medieval open-field system of farming, or a habitational name from a minor place named with this word, such as Furlong in Devon or Shropshire. The surname is now chiefly common in Ireland, where a family of this name settled at the end of the 13th century.Possibly an Americanized form of French Ferland.
Girl/Female
Indian
Stability
Surname or Lastname
English
English : habitational name from either of two places, in Greater Manchester and Merseyside, named from Welsh ynys ‘island’, ‘strip of land between two rivers’ (cf. Innes).
Male
Chinese
stability and fortune.
Girl/Female
Biblical
Preparation, or stability, of the Lord.
Surname or Lastname
English
English : perhaps a habitational name for someone who lived by a long strip of ground, Middle English langet (a derivative of lang ‘long’).
Surname or Lastname
English
English : topographic name for someone who lived on or by a strip of land, Old English strīp.
Surname or Lastname
English
English : variant of Stripling.
Biblical
preparation, or stability, of Jehovah
Surname or Lastname
English
English : habitational name from places in Somerset and Dorset (now part of Bournemouth), probably named with Old English langet ‘long strip of ground’, ‘long ridge’ + dūn ‘hill’.
Male
Greek
Short form of Greek Eustathios, STATHIS means "good stability."
Girl/Female
American, Arabic, Chinese, Danish, Finnish, German, Greek, Indian, Kannada, Marathi, Muslim
Stability; Ocean or Sea; From the Earth; Pure; Earth; Chicken; Hen
Surname or Lastname
English
English : from the medieval personal name Hicke, a pet form of Richard. The substitution of H- as the initial resulted from the inability of the English to cope with the velar Norman R-.Dutch : from a pet form of a Germanic personal name, such as Icco or Hikke (a Frisian derivative of a compound name with the first element hild ‘strife’, ‘battle’).East German : from a derivative of a Slavic pet form of Heinrich.South German : from Hiko, a pet form of any of the Germanic personal names formed with hild ‘strife’, ‘battle’ as the first element.
Girl/Female
Muslim
Stability
INSTABILITY STRIP
INSTABILITY STRIP
Boy/Male
Indian, Sanskrit
Without Anger
Girl/Female
Hindu, Indian, Marathi, Sanskrit, Tamil
Fulfilling; Completing; Another Name for Durga
Biblical
knowledge of Jehovah
Boy/Male
Bengali, Hindu, Indian, Kannada, Marathi, Telugu
Son of the Sun; Sky
Surname or Lastname
English
English : nickname for a small man, or distinguishing epithet for the younger of two bearers of the same personal name, from Middle English littel, Old English l̄tel, originally a diminutive of l̄t (see Light 3).Irish : translation of Gaelic Ó Beagáin ‘descendant of Beagán’ (see Begin).Translation of French Petit and Lepetit; also used as an English form of names such as Jean-Petit ‘little John’.Translation of any of various other European name meaning ‘little’.
Girl/Female
Tamil
Tanvisha | தாநà¯à®µà¯€à®·à®¾
Boy/Male
German
Victorious ruler.
Girl/Female
Latin
Jagged mountain. A mountain in Spain: (Montserrat); a monastery.
Girl/Female
Indian
Honesty, Just, Upright, Justice
Girl/Female
Arabic, Muslim
Reliance; Dependence
INSTABILITY STRIP
INSTABILITY STRIP
INSTABILITY STRIP
INSTABILITY STRIP
INSTABILITY STRIP
n.
Inability to judge.
a.
Uncertainty; instability.
n.
Instability; unstableness.
n.
Inability.
a.
The state or quality of being stable, or firm; steadiness; firmness; strength to stand without being moved or overthrown; as, the stability of a structure; the stability of a throne or a constitution.
pl.
of Instability
n.
Slipperiness; instability; as, the lubricity of fortune.
n.
The quality or condition of being unstable; want of stability, firmness, or steadiness; liability to give way or to fail; insecurity; precariousness; as, the instability of a building.
n.
Strength; stability.
n.
Inability.
n.
Instability; inconstancy.
n.
Inability to swallow.
n.
Lack of determination of fixedness; inconstancy; fickleness; mutability; changeableness; as, instability of character, temper, custom, etc.
n.
Unsuitableness; unaptness; unfitness; inability.
a.
Steadiness or firmness of character, firmness of resolution or purpose; the quality opposite to fickleness, irresolution, or inconstancy; constancy; steadfastness; as, a man of little stability, or of unusual stability.
n.
Strength; firmness; stability.
n.
The quality of being fickle; instability; inconsonancy.
n.
Inability; helplessness.
n.
The quality of turning; instability; tergiversation.
pl.
of Notability