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Mira variable

A Mira variable, also known as a long-period variable, is a type of pulsating asymptotic giant branch (AGB) star that undergoes regular radial pulsations in its fundamental mode, resulting in significant brightness variations over periods ranging from approximately 100 to more than 1000 days, with visual light amplitudes exceeding 2.5 magnitudes.^[1] These stars are typically cool, red giants with spectral types from late K to M (for oxygen-rich variants) or C (for carbon-rich ones), effective temperatures around 2000–3500 K, and luminosities of 1000–10,000 times that of the Sun, marking the final stages of evolution for intermediate-mass stars (0.8–8 M⊙) before they shed their outer envelopes to form planetary nebulae or white dwarfs.^[1]^[2] The class is named after its prototype, Mira (ο Ceti), the first known variable star, discovered on August 3, 1596, by Dutch astronomer David Fabricius, who initially mistook its appearance for a nova due to its dramatic fading; its periodic nature was confirmed by later astronomers, including Johannes Hevelius, who named it Mira (Latin for "wonderful") in 1662.^[1]^[3] Mira variables exhibit complex atmospheric dynamics, including substantial mass loss rates (up to 10⁻⁶ M⊙ yr⁻¹) driven by a κ-mechanism in ionization zones, which powers the pulsations and leads to the formation of dusty circumstellar envelopes that contribute to the interstellar medium.^[2]^[4] Astronomically significant, Mira variables serve as standard candles through their well-defined period–luminosity (P–L) relations, first empirically established in the Large Magellanic Cloud in 1981, allowing precise distance measurements to galaxies in the Local Group and beyond, with recent calibrations using Gaia DR3 data yielding Hubble constant estimates around 72 km s⁻¹ Mpc⁻¹.^[1]^[5] Their study provides insights into late-stage stellar evolution, nucleosynthesis, and galactic chemical enrichment, with ongoing observations revealing subtle variations in pulsation modes and infrared excesses that refine models of AGB physics.^[1]^[2]

History and Discovery

Discovery of Mira

The discovery of the first Mira variable began with observations by the German astronomer David Fabricius in 1596, who first noted the star—now designated Omicron Ceti—on August 3 while searching for Mercury near the constellation Cetus with the naked eye.^[3] Fabricius described it as a previously uncharted star of about third magnitude, positioned between two known stars, Zeta and Eta Ceti, and remarked on its irregular brightness fluctuations over subsequent nights, fading to near invisibility by late August.^[6] His son, Johann Fabricius, independently confirmed these observations later that same year, contributing to early records of the star's anomalous behavior in their 1603 publication De Stella Nova in Collo Ceti.^[6] Interest in the star waned until the mid-17th century, when Polish astronomer Johannes Hevelius began systematic monitoring in 1648, compiling extensive data on its cyclic changes over more than three decades.^[7] In his 1662 treatise Historiola Mirae Stellae, Hevelius formally named it "Mira" (Latin for "wonderful"), highlighting its dramatic variability as a phenomenon unlike any other known star at the time.^[8] Hevelius's work emphasized the star's recurrent appearances and disappearances, which he tracked meticulously against fixed reference stars. In 1638, prior to Hevelius's systematic observations, Johannes Holwarda had determined Mira's period to be approximately 11 months (332 days), establishing it as the first recognized periodic variable star.^[3] By the mid-17th century, accumulated observations from Fabricius, Holwarda, Hevelius, and others had revealed a pulsation period of approximately 332 days, during which Mira's visual magnitude swung from about 2 at maximum—making it visible to the naked eye—to around 10 at minimum, rendering it effectively invisible without aid.^[9] These findings established Omicron Ceti as the prototype for what would later be recognized as a distinct class of long-period variable stars.^[3]

Classification and Naming

In the 19th century, astronomers including John Herschel recognized a class of pulsating red giant stars characterized by extended variability cycles, referring to them as "variable stars of long period" and advocating for their systematic observation by amateurs.^[10] This informal grouping laid the groundwork for later formalization, building on the 17th-century discovery of the prototype Mira (ο Ceti) as the first known periodic variable.^[11] The modern classification was established in the General Catalogue of Variable Stars (GCVS), where Mira (Omicron) Ceti-type variables are defined as long-period variable giants with late-type emission spectra (Me, Ce, Se) and light amplitudes from 2.5 to 11 magnitudes in the V-band, with periods between 80 and 1000 days, distinguishing them from shorter-period or lower-amplitude pulsators.^[12]^[13] The GCVS, maintained under the auspices of the International Astronomical Union (IAU) Commission 27 on Variable Stars, formalized this category in the mid-20th century, emphasizing the stars' regular, large-amplitude pulsations.^[14] Further refinements by the IAU in the 20th century delineated Mira variables from semiregular variables (SR types) based on greater periodicity and amplitude stability, with Miras exhibiting more consistent cycles and variations typically between 2.5 and 10 magnitudes, while SR stars show smaller amplitudes under 2.5 magnitudes and less defined regularity.^[11] The naming convention derives from the prototype Mira, with the class termed "Mira variables"; subtypes include oxygen-rich Mira M stars (C/O ≤ 1) and carbon-rich Mira C stars (C/O > 1), reflecting differences in atmospheric composition.^[15]^[16]

Physical Characteristics

Stellar Parameters

Mira variables are evolved stars on the asymptotic giant branch (AGB) with typical masses ranging from 0.5 to 2 solar masses (M⊙), reflecting their origins as low- to intermediate-mass progenitors that have exhausted core hydrogen and helium burning.^[17] These stars exhibit enormous sizes, with radii spanning 100 to 1000 solar radii (R⊙), which contribute to their extended, distended structures and significant pulsational behavior.^[18] Their luminosities are correspondingly high, typically between 10³ and 10⁴ solar luminosities (L⊙), driven by the energy release from shell burning in the hydrogen- and helium-rich layers surrounding the degenerate core.^[1] The spectral types of Mira variables are predominantly late-type, ranging from M3 to M9 for oxygen-rich examples, corresponding to cool effective temperatures of approximately 2500 to 3500 K that favor the formation of metal oxide bands like TiO and VO in their atmospheres.^[19] A subset consists of carbon-rich Mira variables with C-type spectra, where carbon dredged up from the interior exceeds oxygen abundance, leading to features from CN and C₂ molecules.^[18] Surface gravities are low, with log g ≈ 0 (in cgs units), indicative of their supergiant-like expansion and reduced density compared to less evolved giants.^[20] Chemically, Mira variables display enrichments in s-process elements—such as barium, strontium, and zirconium—resulting from neutron capture nucleosynthesis in the thermal pulses of the AGB phase, followed by third dredge-up episodes that mix these products to the surface.^[1] This enrichment, alongside enhancements in carbon or heavy metals depending on the subtype, underscores their role as contributors to galactic chemical evolution. Periods of 100 to 1000 days serve as a defining observational characteristic, linking these parameters to their pulsation dynamics.^[1]

Atmospheric and Envelope Properties

Mira variables possess extended, thick atmospheres characterized by significant molecular content, which contributes to their distinctive red colors and spectral features. These atmospheres feature prominent absorption bands from titanium oxide (TiO) and water vapor (H₂O), with TiO bands dominating the optical spectrum shortward of 1 μm and causing deep absorptions that enhance the reddish appearance of these stars.^[21] The optically thick H₂O layers in the extended atmosphere lead to emission filling in absorption lines, resulting in relatively featureless continuum-like spectra in the mid-infrared, such as around 11 μm.^[22] These molecular bands arise in layers extending several stellar radii from the photosphere, influencing the overall energy distribution and making Mira variables appear larger in angular size at longer wavelengths compared to the near-infrared.^[22] Surrounding the star, Mira variables develop circumstellar envelopes through ongoing mass loss, a hallmark of their asymptotic giant branch (AGB) phase. These envelopes consist of gas and dust ejected at expansion velocities typically ranging from 5 to 20 km/s, with an average terminal velocity of about 7 km/s observed in nearby examples.^[23] Dust shells within these envelopes are particularly prominent in the infrared, where they re-emit absorbed stellar radiation, rendering the stars bright at wavelengths beyond 10 μm and often obscuring the central star in the optical for the dustiest cases.^[23] Infrared observations reveal these shells as extended structures, with angular sizes increasing with wavelength due to the dust's thermal emission.^[22] Molecular layers in the inner circumstellar envelopes host maser emissions from species like silicon monoxide (SiO), hydroxyl (OH), and H₂O, which are detectable at radio wavelengths. SiO masers, for instance, form in ring-like structures at radii of 1.8 to 2.4 times the infrared photospheric radius, pumped by radiative and collisional processes in the shocked, optically thick gas.^[24] These masers trace the dynamics of the envelope's inner regions, with emissions peaking at specific pulsation phases and exhibiting velocity widths of around 10 km/s.^[24] OH and H₂O masers extend farther out, up to several hundred stellar radii, providing insights into the envelope's stratified molecular composition and expansion.^[25]

Pulsation and Variability

Pulsation Mechanism

Mira variables are asymptotic giant branch (AGB) stars that exhibit large-amplitude radial pulsations sustained by the κ-mechanism within the ionization zones of hydrogen and helium in the extended convective envelope. These pulsations occur on timescales of hundreds of days, while underlying thermal pulses from periodic helium shell flashes—arising when accumulated helium in the thin shell around the degenerate carbon-oxygen core ignites—drive longer-term evolutionary changes, including variations in the pulsation period.^[26]^[2] The observed pulsations manifest as radial oscillations primarily in the fundamental mode (though the exact mode—fundamental or first overtone—remains debated in the literature), sustained by the κ-mechanism. In the compression phase, rising temperature and density increase opacity, impeding radiative energy outflow and leading to localized heating that enhances the subsequent expansion phase.^[27]^[28] Energy transport in these cool giants occurs predominantly via convection in the outer layers, with radiative diffusion contributing in deeper regions; variations in opacity due to molecular and ionization effects further amplify the pulsational instability by modulating heat retention.^[26] The pulsation period P relates to the stellar structure through the approximate dynamical timescale formula for the fundamental mode:

P \approx Q \sqrt{\frac{R^3}{GM}},

where R is the stellar radius, M is the mass, G is the gravitational constant, and Q is the pulsation constant typically around 0.08–0.10 days for Mira variables.^[27] These interior dynamics produce characteristic light variations with periods longer than 100 days.

Light and Spectral Variations

Mira variables exhibit distinctive asymmetric light curves characterized by a rapid rise in brightness followed by a prolonged decline. The rise phase typically occupies 10-20% of the pulsation period, reflecting the dynamic expansion of the stellar atmosphere, while the decline spans the remaining duration as the star contracts more gradually. In the visual band, these variations produce amplitudes ranging from 4 to 10 magnitudes, with classical examples like Mira (o Ceti) showing changes of about 8-9 magnitudes.^[29]^[30] Accompanying these photometric changes are pronounced spectral variations driven by pulsation-induced temperature fluctuations. Effective temperatures range from approximately 3000 K at maximum light, when the spectrum appears earlier in type (e.g., M5), to around 2400 K at minimum, shifting to later types (e.g., M8-M9). This cooling enhances the formation of metal oxide molecules, notably deepening the absorption bands of titanium oxide (TiO) in the optical spectrum during the decline phase, which can significantly obscure the continuum flux at minimum light. Vanadium oxide (VO) bands also strengthen similarly, contributing to the redder appearance at fainter phases.^[31]^[2]^[32] Radial velocity measurements further confirm the radial pulsation mode, with curves approximating a sinusoidal profile phased to the light variation. Semi-amplitudes typically fall between 20 and 50 km/s, as observed in infrared CO and OH lines that probe deeper atmospheric layers; for instance, R Leonis displays an amplitude of 27 km/s. These velocities indicate pulsational motions extending to the photosphere, with maxima approaching during the rise to brightness maximum.^[4]

Evolutionary Role

Position in AGB Evolution

Mira variables represent a key evolutionary stage for low- to intermediate-mass stars (approximately 0.8–8 M⊙) during the asymptotic giant branch (AGB) phase, specifically within the thermally pulsing AGB (TP-AGB) regime. This phase commences after the exhaustion of core helium burning, when the star's evolution is dominated by hydrogen shell burning surrounding a degenerate helium core, leading to rapid luminosity increases and the star's ascent along the AGB in the Hertzsprung-Russell diagram. The TP-AGB is characterized by periodic thermal pulses in the helium-burning shell, which ignite under degenerate conditions and drive convective mixing events known as third dredge-ups, enriching the stellar surface with processed material. These thermal pulses occur on timescales of interpulse periods ranging from 10⁴ to 10⁵ years, during which quiescent hydrogen shell burning predominates and the star maintains a relatively stable structure interrupted only by the brief pulse phases lasting hundreds of years. Mira variables embody the classical AGB stage in this context, where the star's envelope expands to low effective temperatures (around 3000 K) and high luminosities (10³–10⁴ L⊙), fostering conditions for large-amplitude radial pulsations driven by the kappa-mechanism, with shocks propagating through the atmosphere during pulsation cycles. This pulsation regime distinguishes Miras as fundamental-mode pulsators before the onset of more extreme mass-loss episodes. As evolution progresses within the TP-AGB, increasing mass loss gradually erodes the envelope, culminating in a superwind phase that marks the end of the Mira variability. This transition propels the star off the AGB, ionizing the ejected material and forming a proto-planetary nebula, thereby concluding the Mira phase and initiating the post-AGB evolution toward a white dwarf remnant.

Period Changes and Mass Loss

Mira variables exhibit secular changes in their pulsation periods, observed in approximately 10% of the population at a significance level of 2σ or greater, based on analyses of long-term photometric data from hundreds of stars. These changes, quantified as rates d ln P/dt ranging from about -8 × 10^{-3} to +6 × 10^{-3} yr^{-1}, correspond to dP/dt values typically on the order of 10^{-2} to 1 days per year for periods around 300 days, with extremes up to several days per year, though the median for changing stars is roughly 1.5 × 10^{-3} yr^{-1} in d ln P/dt. Such variations are attributed to evolutionary processes during the thermally pulsing asymptotic giant branch (TP-AGB) phase, including core contraction that shortens the period or envelope expansion due to thermal pulses that lengthen it.^[33] Mass loss in Mira variables occurs at rates spanning 10^{-7} to 10^{-4} M_\odot yr^{-1}, with higher rates associated with longer-period stars and more luminous envelopes. This process is primarily driven by stellar pulsations, which extend the atmosphere and promote dust grain formation at distances of 3–10 stellar radii, followed by acceleration of the outflow via radiation pressure on the dust. The pulsation-enhanced levitation creates conditions for efficient dust condensation, leading to a dust-driven wind that ejects material at terminal velocities v_\exp of 5–20 km s^{-1}. Observations of CO emission lines from circumstellar envelopes confirm these rates, with the total mass loss contributing significantly to the interstellar medium enrichment. Recent studies indicate that third dredge-up events can influence mass loss rates by altering surface composition and dust properties, particularly in carbon-rich Miras.^[34]^[35] The mass loss rate \dot{M} is related to the stellar luminosity L and expansion velocity v_\exp by the approximate relation \dot{M} \propto L / v_\exp, derived from momentum transfer in the dust-driven wind where radiation pressure balances the outflow. This scaling arises because the momentum imparted by stellar photons on dust grains (proportional to L/c) drives the gas-dust mixture, with v_\exp setting the efficiency. Enhanced mass loss manifests observationally as infrared excesses from re-emitted thermal radiation by the circumstellar dust envelope, detectable in mid- to far-infrared surveys and correlating with period and luminosity.^[36]

Notable Examples

Mira (Omicron Ceti)

Mira, also known as Omicron Ceti, is the prototypical Mira variable star and the namesake of its class, serving as a benchmark for understanding long-period pulsations in asymptotic giant branch stars. This binary system consists of the pulsating red giant Mira A and a compact companion Mira B, located approximately 300 light-years (92 parsecs) away, as measured by Gaia DR3 parallax measurements.^[37] The primary star exhibits a pulsation period of 331.8 days, during which its visual brightness varies by an amplitude of about 8.6 magnitudes, ranging from roughly magnitude 3.4 at maximum to 10.0 at minimum. Its spectral type shifts between M5e and M9e across the cycle, reflecting changes in temperature and atmospheric emission lines due to the expanding envelope.^[6] The companion, Mira B, was identified as a hot white dwarf in observations from 2005, orbiting Mira A with an orbital period of approximately 500 years and influencing the system's dynamics through interactions with the stellar wind.^[38]^[37] Mira A exhibits historical changes in its pulsation period on timescales of decades, reflecting complex dynamics in its evolution.^[27] Material from Mira A's stellar wind accretes onto Mira B, powering occasional X-ray emissions detected in the system, primarily from the boundary layer of the accretion disk around the white dwarf.^[39] Mira exhibits strong SiO maser emission in its circumstellar envelope, arising from silicon monoxide molecules in the shocked layers near the photosphere, which trace the pulsation-driven outflows with high intensity at millimeter wavelengths.^[40] Additionally, the system's high space velocity of about 130 km/s relative to the local interstellar medium produces a prominent bow shock, first imaged in ultraviolet by GALEX in 2005, where the stellar wind compresses ambient gas into an arc-like structure ahead of the motion.^[41] These features highlight Mira's role as a dynamic laboratory for studying mass loss and binary interactions in evolved stars.

Other Prominent Mira Variables

R Leporis, commonly known as Hind's Crimson Star, exemplifies carbon-rich Mira variables with a pulsation period of approximately 430 days and a visual magnitude range from 5.5 to 11.7.^[42] Its intensely red appearance stems from molecular bands of carbon compounds in its atmosphere, marking it as a C-type star where carbon exceeds oxygen abundance. Observations with the Atacama Large Millimeter/submillimeter Array (ALMA) have revealed a detailed circumstellar envelope surrounding the star, composed of complex carbon-bearing molecules and dust, extending to reveal the star's mass-loss history at unprecedented resolution.^[44] Chi Cygni represents an S-type Mira variable, transitional between oxygen-rich and carbon-rich compositions, with a pulsation period of about 408 days and a typical visual amplitude of around 6 magnitudes, though extremes reach up to 10 magnitudes from 3.3 to 14.2.^[45] Its spectrum shows zirconium oxide bands characteristic of S stars, and millimeter-wave observations indicate variable molecular emissions in the inner envelope, reflecting dynamic pulsation-driven chemistry.^[46] R Carinae demonstrates extreme variability among Mira stars, with a period of approximately 309 days and a visual amplitude of about 7 magnitudes, ranging from 3.9 to 10.5.^[47] This oxygen-rich star has been instrumental in early calibrations of the period-luminosity relation for Mira variables, helping establish their use as standard candles for galactic distance measurements.^[48] Like other prominent examples, it exhibits the characteristic red hues and long-period pulsations typical of the class.

Scientific Significance

Observational Techniques

Observational techniques for Mira variables leverage their predictable pulsation cycles to synchronize multi-wavelength campaigns, capturing the full range of atmospheric and circumstellar phenomena over periods of hundreds of days.^[49] Photometric monitoring forms the cornerstone of Mira variable studies, with long-term light curves constructed from visual observations by amateur and professional networks. The American Association of Variable Star Observers (AAVSO) maintains extensive databases of Mira light curves spanning decades, enabling analysis of amplitude, period, and cycle-to-cycle irregularities in the visual band. To probe dust formation and its impact on the stellar environment, photometry extends across ultraviolet (UV) to infrared (IR) filters; UV observations reveal absorption by newly formed dust grains, while IR data track thermal re-emission from circumstellar shells, as demonstrated in studies of carbon-rich Miras where dust obscuration correlates with mass-loss episodes. High-resolution spectroscopy provides insights into atmospheric dynamics through measurements of radial velocities from absorption lines of metals like iron and titanium oxides. Time-series spectra along the pulsation cycle yield velocity amplitudes exceeding 20 km/s, mapping the expansion and contraction of the extended atmosphere.^[49] Complementary spectroscopic techniques target circumstellar masers, with very long baseline interferometry (VLBI) using arrays like the Very Long Baseline Array (VLBA) to map SiO maser emissions at 43 GHz, revealing ring-like distributions around the star at distances of 10-20 stellar radii and tracing mass outflows. Interferometric observations directly resolve the stellar surface and atmosphere, measuring angular diameters in the near-infrared where molecular opacity is lower. Facilities such as the Very Large Telescope Interferometer (VLTI) and the Center for High Angular Resolution Astronomy (CHARA) Array have yielded uniform-disk angular diameters of 5-20 milliarcseconds for nearby Miras, corresponding to physical radii of approximately $500 \, R_\odot at maximum light phase, after combining with distance estimates from period-luminosity relations.^[50] These measurements confirm the extended photospheres predicted by dynamic atmosphere models and highlight asymmetries due to convection and shocks.^[51]

Astrophysical Applications

Mira variables serve as valuable distance indicators in astrophysics due to their well-defined period-luminosity relation (PLR), which correlates the pulsation period with intrinsic luminosity, enabling precise measurements of distances to galaxies in the Local Group and beyond, much like Cepheid variables. This relation has been calibrated using geometric distances to the Large Magellanic Cloud and trigonometric parallaxes from Gaia, allowing for applications such as determining the distance to the Galactic center at approximately 8.2 kpc and to galaxies like M101 with uncertainties as low as 4%.^[52]^[53] By extending the cosmic distance ladder, Mira PLRs contribute to independent estimates of the Hubble constant, with recent calibrations from globular cluster Miras yielding values around 73 km/s/Mpc.^[54] Asymptotic giant branch (AGB) stars, including Mira variables, are key sites for s-process nucleosynthesis, where slow neutron capture produces heavy elements beyond iron, such as barium and strontium, which are dredged up to the stellar surface and ejected into the interstellar medium (ISM). Observations of enhanced s-process signatures in Mira spectra confirm their role in enriching the ISM, with models showing that AGB stars contribute up to 50-70% of s-process elements in solar metallicity environments.^[55]^[56] Additionally, Mira variables drive significant dust production through radiative acceleration of circumstellar grains, releasing silicates and carbon dust at rates of 10^{-8} to 10^{-6} M_\sun per year, which seeds molecular cloud formation and influences galactic chemical evolution.^[57] Studies of Mira variables provide critical calibrations for models of late stellar evolution, particularly in quantifying mass-loss rates that determine the transition to planetary nebulae (PNe) and the resulting white dwarf progenitors. Empirical mass-loss prescriptions, derived from Mira observations, indicate rates increasing with pulsation period and luminosity, up to 10^{-4} M_\sun yr^{-1} near the AGB tip, which sculpt the progenitors' envelopes and set the initial-to-final mass relation for white dwarfs around 0.5-0.6 M_\sun.^[58]^[59] These calibrations refine hydrodynamic simulations of PNe formation, ensuring accurate predictions of nebular morphologies and the chemical yields returned to the ISM.^[60]

References

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### Summary for Encyclopedia Intro: Mira Variables
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An informal review of the problems of understanding Mira variables has been given by Wing (1980). Mira stars are the subset of pulsating giant stars which have ...
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The structure of Mira variables can perhaps best be described as loose. They are enormous, distended stars, and it is clear that many differ- ent atmospheric ...
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A period–luminosity relation for Mira variables in the Large ... - Nature
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Omicron Ceti (Mira) - aavso
David Fabricius of East Friesland, Germany is recognized to have discovered OMICRON CETI in 1596 while searching for Mercury. ... Within the first century ...
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History of the Discovery of Mira Stars - Astrophysics Data System
Within the first century following Fabricius, four Mira-type variables were discovered, and in all cases it has been found that the stars were suspected of ...
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Who Discovered Mira Ceti? (The first variabilist was a Celt man who ...
The name Mira was attributed to it definitely by Johannes Hevelius, who had taken regular observations of omicron Ceti since 1 648 and inserted it in his ...
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Mira a 'Wonderful' Maximum - British Astronomical Association
Jan 9, 2018 · On the morning of August 3rd, 1596, German astronomer David Fabricius used an unmarked third magnitude star in Cetus as a reference point ...
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proved to be both a lengthy and difficult task in the 19th Century. As early as. 1833 Sir John Herschel advocated that amateur astronomers take up variable star.
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[PDF] Amplitude Variations in Pulsating Red Giants - aavso
Pulsating red giants are classified in the General Catalogue of Variable. Stars (GCVS; Kholopov et al. 1985) as Mira (M) variables if their visual amplitude is ...
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[PDF] Comparison of dynamical model atmospheres of Mira variables with ...
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[PDF] A CO(3{2) Survey of Nearby Mira Variables - arXiv
ABSTRACT. A survey of CO(3–2) emission from optically visible oxygen–rich Mira variable stars within 500 pc of the sun was conducted.
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[PDF] SiO Maser Emission in Miras - arXiv
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Mira—periodic red giant variables with periods ranging from 80 to 1,000 days and visual light variations of more than 2.5 magnitudes. Semiregular—giants and ...
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Mira Variables - OGLE Atlas of Variable Star Light Curves
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"Wonderful" Star Reveals its Hot Nature :: April 28, 2005
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Mira Variables explained by a planetary companion interaction
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X-RAYS FROM THE MIRA AB BINARY SYSTEM - IOP Science
If the X-rays arise from accretion onto Mira B, then the modest X-ray lu- minosity of the system appears to rule out the possibility that. Mira B is a white ...
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Phillips & Boboltz, SiO Masers toward Mira - IOP Science
Delay solutions from the continuum calibrators were applied to the Mira data, and fringe fitting performed on several strong features in the cross power spectra ...
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IT'S A WONDERFUL TAIL: THE MASS-LOSS HISTORY OF MIRA
Nov 6, 2007 · Right: Mosaicked UV images of the Mira AB tail and bow shock. This figure is an adaptation of Fig. 1a from Martin et al. (2007). Please ...
[38]
R Leporis - Carbon Star - Focal Pointe Observatory
Its magnitude varies from +5.5 to +11.7, with a period of 427 days. Being a carbon star, it appears distinctly red. As the star dims it becomes visually redder.
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[40]
khi Cygni | aavso
Khi Cygni the variable. Khi Cygni is a pulsating variable, as are all Mira variables. Their surfaces move periodically in and out, changing the star's ...
[41]
[2408.17000] Millimetre observations of the S-type AGB star $χ$ Cygni
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[42]
[PDF] Citizen Science with Variable Stars - aavso
R Carinae. (R Car). December to August. 3.9 – 10.5. Mira. 307. R Carinae has to be observed with 3 different instruments if you want to cover its entire cycle ...
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Joint VLBA/VLTI Observations of the Mira Variable S Orionis - arXiv
Oct 8, 2004 · Abstract: We present the first coordinated VLBA/VLTI measurements of the stellar diameter and circumstellar atmosphere of a Mira variable star.<|control11|><|separator|>
[46]
Joint VLBA/VLTI Observations of the Mira Variable S Orionis
Our coordinated VLBA/VLTI measurements show that the masers lie relatively close to the stellar photosphere at a distance of ~2 photospheric radii, consistent ...
[47]
[1808.01294] The Mira-based distance to the Galactic centre - arXiv
Aug 3, 2018 · Mira variables are useful distance indicators, due to their high luminosities and well-defined period-luminosity relation. We select 1863 Miras ...
[48]
The Mira Distance to M101 and a 4% Measurement of H0 - arXiv
Dec 13, 2023 · We adopt absolute calibrations of the Mira Period-Luminosity Relation based on geometric distances to the Large Magellanic Cloud and the water ...
[49]
Absolute Calibration of Cluster Mira Variables to Provide a New ...
Jul 14, 2025 · This paper uses Mira variables in globular clusters to calibrate period-luminosity relations, determine the Hubble constant, and provides a 3.7 ...
[50]
Abia et al., s-Process Nucleosynthesis in Carbon Stars - IOP Science
In the present work we have extended our study of s-element nucleosynthesis in N stars to the nuclei belonging to the second s-process peak: Ba, La, Ce, Nd, and ...
[51]
Super and massive AGB stars – III. Nucleosynthesis in metal-poor ...
Abstract. We present a new grid of stellar models and nucleosynthetic yields for super-AGB stars with metallicities Z = 0.001 and 0.0001, applicable for us.
[52]
Gas and dust from metal-rich AGB stars - Astronomy & Astrophysics
Models of nucleosynthesis and dust formation for AGB stars of super-solar ... This distribution, which is relevant to the s-process nucleosynthesis and ...
[53]
Mass loss of stars on the asymptotic giant branch
Jan 9, 2018 · It is during the thermally pulsing stage (TP-AGB) that AGB stars produce a large fraction of the elements we find in the universe, and the ...
[54]
An empirical formula for the mass-loss rates of dust-enshrouded red ...
The mass-loss rates reached by more luminous AGB stars are higher than those reached by less luminous AGB stars, but there is a lot of intrinsic scatter in the ...
[55]
Tracers of stellar mass loss – I. Optical and near-IR colours and ...
It determines the white dwarf mass spectrum and cooling times, and the minimum supernova (SN) progenitor mass. Mass loss thus influences the rate of Types II, ...