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Semiregular variable star
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In astronomy, a semiregular variable star, a type of variable star, is a giant or supergiant of intermediate and late (cooler) spectral type. It shows considerable periodicity in its light changes, accompanied or sometimes interrupted by various irregularities. Periods lie in the range from 20 to more than 2000 days, while the shapes of the light curves may be rather different and variable with each cycle. The amplitudes may be from several hundredths to several magnitudes (usually 1-2 magnitudes in the V filter).
Classification
[edit]The semiregular variable stars have been sub-divided into four categories for many decades, with a fifth related group defined more recently. The original definitions of the four main groups were formalised in 1958 at the tenth general assembly of the International Astronomical Union (IAU). The General Catalogue of Variable Stars (GCVS) has updated the definitions with some additional information and provided newer reference stars where old examples such as S Vul have been re-classified.
| Subtype[1] | IAU definition[1] | GCVS code[2] | GCVS definition[2] | Standard stars |
|---|---|---|---|---|
| SRa | semi-regular variable giants of late spectral classes (M, C and S), which retain periodicity with comparative stability and possess, as a rule, small (less than 2m.5) light-variation amplitudes. Amplitudes and forms of light curves are usually liable to strong variations from period to period. Many of these stars differ from Mira Ceti type stars only owing to the smaller amplitude of light variation. | SRA | Semiregular late-type (M, C, S or Me, Ce, Se) giants displaying persistent periodicity and usually small (<2.5 mag in V) light amplitudes. Amplitudes and light-curve shapes generally vary and periods are in the range of 35–1200 days. Many of these stars differ from Miras only by showing smaller light amplitudes | Z Aqr[1][2] |
| SRb | semi-regular variable giants of late spectral classes (M, C and S) with a poorly expressed periodicity, i.e. with a different duration of individual cycles (which leads to the impossibility of predicting the epochs of maximum and minimum brightness), or with the replacement of periodical changes by slow irregular variations, or even by the constancy of brightness. Some of them are characterised by a certain mean value of the period, given in the catalogue. | SRB | Semiregular late-type (M, C, S or Me, Ce, Se) giants with poorly defined periodicity (mean cycles in the range of 20 to 2300 days) or with alternating intervals of periodic and slow irregular changes, and even with light constancy intervals. Every star of this type may usually be assigned a certain mean period (cycle), which is the value given in the Catalogue. In a number of cases, the simultaneous presence of two or more periods of light variation is observed | AF Cyg[1][2] RR CrB[1][2] |
| SRc | semi-regular variable super-giants of late spectral classes | SRC | Spectral-type (M, C, S or Me, Ce, Se) supergiants with amplitudes of about 1 mag and periods of light variation from 30 days to several thousand days. | μ Cep[1][2] RW Cyg[1] |
| SRd | semi-regular variable giants and super-giants belonging to spectral classes F, G, K | SRD | Semiregular variable giants and supergiants of F, G, or K spectral types, sometimes with emission lines in their spectra. Amplitudes of light variation are in the range from 0.1 to 4 mag, and the range of periods is from 30 to 1100 days | S Vul[1] UU Her[1] AG Aur[1] SX Her[2] SV UMa[2] |
| SRS | Semiregular pulsating red giants with short period (several days to a month), probably high-overtone pulsators | AU Ari[2] |
Pulsation
[edit]The semiregular variable stars, particularly the SRa and SRb sub-classes, are often grouped with the Mira variables under the long-period variable heading. In other situations, the term is expanded to cover almost all cool pulsating stars. The semi-regular giant stars are closely related to the Mira variables: Mira stars generally pulsate in the fundamental mode; semiregular giants pulsate in one or more overtones.[3]
Photometric studies in the Large Magellanic Cloud looking for gravitational microlensing events have shown that essentially all cool evolved stars are variable, with the coolest stars showing very large amplitudes and warmer stars showing only micro-variations. The semiregular variable stars fall on one of five main period-luminosity relationship sequences identified, differing from the Mira variables only in pulsating in an overtone mode. The closely related OSARG (OGLE small amplitude red giant) variables pulsate in an unknown mode.[4][5]
Many semiregular variables show long secondary periods around ten times the main pulsation period, with amplitudes of a few tenths of a magnitude at visual wavelengths. The cause of the pulsations is not known.[3]
Bright examples
[edit]η Gem is the brightest SRa variable, and also an eclipsing binary. GZ Peg is an SRa variable and S-type star with a maximum magnitude of 4.95. T Cen is listed as the next-brightest SRa example,[2] but it is suggested that it may actually be an RV Tauri variable, which would make it by far the brightest member of that class.[6]
There are numerous naked-eye SRb stars, with third-magnitude L2 Pup being the brightest listed in the GCVS. σ Lib and ρ Per are also third-magnitude SRb stars at maximum brightness. β Gru is a second magnitude star classified as a slow irregular variable by the GCVS, but reported to be of SRb type by later research.[7] These four are all class M giants, although some SRb variables are carbon stars such as UU Aur or S-type stars such as Pi1 Gru.[2]
Catalogued SRc stars are less numerous, but include some of the brightest stars in the sky such as Betelgeuse and α Her. Although SRc stars are defined as being supergiants, a number of them have giant spectral luminosity classes and some such as α Her are known to be asymptotic giant branch stars.[2]
Many SRd stars are extremely luminous hypergiants, including the naked-eye ρ Cas, V509 Cas, and ο1 Cen. Others are classified as giant stars, but the brightest example is the seventh-magnitude LU Aqr.[2]
Most SRS variables have been discovered in deep large-scale surveys, but the naked-eye stars V428 And, AV Ari, and EL Psc are also members.[2]
See also
[edit]References
[edit]- ^ a b c d e f g h i j Kukarkin, B. V. (2016). "27. Commission des Etoiles Variables". Transactions of the International Astronomical Union. 10: 398–431. doi:10.1017/S0251107X00020988.
- ^ a b c d e f g h i j k l m n "GCVS Variability Types". General Catalogue of Variable Stars @ Sternberg Astronomical Institute, Moscow, Russia. 12 Feb 2009. Retrieved 2010-11-24.
- ^ a b Nicholls, C. P.; Wood, P. R.; Cioni, M.-R. L.; Soszyński, I. (2009). "Long Secondary Periods in variable red giants". Monthly Notices of the Royal Astronomical Society. 399 (4): 2063. arXiv:0907.2975. Bibcode:2009MNRAS.399.2063N. doi:10.1111/j.1365-2966.2009.15401.x. S2CID 19019968.
- ^ Soszyński, I.; Udalski, A.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Wyrzykowski, Ł.; Szewczyk, O.; Ulaczyk, K.; Poleski, R. (2009). "The Optical Gravitational Lensing Experiment. The OGLE-III Catalog of Variable Stars. IV. Long-Period Variables in the Large Magellanic Cloud". Acta Astronomica. 59 (3): 239. arXiv:0910.1354. Bibcode:2009AcA....59..239S.
- ^ Soszynski, I.; Dziembowski, W. A.; Udalski, A.; Kubiak, M.; Szymanski, M. K.; Pietrzynski, G.; Wyrzykowski, L.; Szewczyk, O.; Ulaczyk, K. (2007). "The Optical Gravitational Lensing Experiment. Period--Luminosity Relations of Variable Red Giant Stars". Acta Astronomica. 57: 201. arXiv:0710.2780. Bibcode:2007AcA....57..201S.
- ^ Watson, C. L. (2006). "The International Variable Star Index (VSX)". The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23–25. 25: 47. Bibcode:2006SASS...25...47W.
- ^ Otero, S. A.; Moon, T. (December 2006). "The Characteristic Period of Pulsation of β Gruis". The Journal of the American Association of Variable Star Observers. 34 (2): 156–164. Bibcode:2006JAVSO..34..156O.
External links
[edit]- EU Delphini and the Small-Amplitude Pulsating Red Giants
- Y Lyncis
- Pulsating variable stars and the H-R diagram
- OGLE Atlas of Variable Star Light Curves - Semiregular Variables
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Semiregular variable star
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Semiregular variable stars are giant or supergiant stars of intermediate and late spectral types, such as M, C, and S, that exhibit brightness variations with noticeable but often irregular periodicity due to radial pulsations in their extended envelopes. These variations typically have periods ranging from 20 days to more than 2000 days and visual amplitudes of several hundredths to several magnitudes, usually 1–2 magnitudes, with light curves that can differ significantly in shape.[1]
The General Catalogue of Variable Stars (GCVS) classifies semiregular variables into several subclasses to account for differences in spectral type, regularity of pulsation, and evolutionary status. SRa stars are late-type giants (M, C, S, and their emission-line variants) with persistent periodicity, amplitudes less than 2.5 magnitudes in V, and periods of 35–1200 days; SRb are similar giants but with poorly defined or alternating periodic and irregular changes, periods of 20–2300 days; SRc are late-type supergiants with amplitudes around 1 magnitude and periods from 30 days to several thousand days; SRd encompass F, G, or K giants and supergiants, often with emission lines, amplitudes of 0.1–4 magnitudes, and periods of 30–1100 days; and SRs are short-period (days to a month) red giants likely pulsating in high overtones.[1] These subclasses highlight the diversity within the group, where fundamental-mode pulsations dominate in more regular cases akin to Mira variables, while multi-periodic or chaotic behavior occurs in others due to overlapping pulsation modes or stochastic processes.[2]
Notable examples include Betelgeuse (α Orionis), a red supergiant classified as SRc with a primary period of about 400 days and amplitudes up to 1.5 magnitudes, and Antares (α Scorpii), a slow irregular variable (LC) red supergiant in the Hertzsprung-Russell diagram.[3][4] Other prominent semiregular variables are L2 Puppis, an SRa star showing complex light curves indicative of evolutionary transitions, and μ Cephei, a hypergiant with irregular outbursts.[5]
Semiregular variables represent a critical phase in the asymptotic giant branch (AGB) evolution of low- to intermediate-mass stars, marking the onset of significant mass loss through stellar winds and providing insights into the dynamical atmospheres of evolved stars. Their pulsations drive dust formation and circumstellar envelopes, influencing galactic chemical enrichment, and while less precise than Miras for distance measurements, they serve as standard candles in nearby galaxies and probes of stellar structure models.[2]
with as the radius, the gravitational constant, and the mass, linking observable variability to underlying stellar structure.[33]
Overview
Definition
Semiregular variable stars are giant or supergiant stars of intermediate and late spectral types, including M, C, and S classes, that display periodic light variations which are not strictly regular.[6] These stars exhibit noticeable periodicity in their brightness changes, often interrupted by intervals of semiregular or irregular fluctuations, setting them apart from other variable star classes.[6] The defining characteristic of semiregular variables is their quasi-periodic or multi-periodic behavior, where light curves show appreciable repetition but lack the precise regularity seen in types like Cepheids.[7] This irregularity arises from complex interactions in their atmospheres and envelopes, leading to variations that can include multiple overlapping cycles.[6] Primarily, semiregular variables consist of asymptotic giant branch (AGB) stars or red supergiants, representing evolved, cool luminous phases in stellar evolution.[7] Their pulsations, driven by internal thermal instabilities, are the general cause of these light variations.[6]General Characteristics
Semiregular variable stars exhibit light variations with amplitudes ranging from 0.01 magnitudes to several magnitudes, though commonly 1–2 magnitudes in the V filter.[6] Their periods span from 20 days to over 2000 days, frequently displaying multiple overlapping periods or intervals of irregularity that result in non-repeating light curves suggestive of superimposed pulsation modes.[1][8] These photometric traits distinguish them from more regular pulsators like Mira variables, which have larger amplitudes and stricter periodicity.[2] Spectrally, semiregular variables are predominantly giants or supergiants of late spectral types, including M, C, and S classes, characterized by prominent molecular absorption bands such as titanium oxide (TiO) in M-type giants.[8] Earlier subtypes, like those in F, G, or K classes, may show weaker or occasional TiO features alongside metallic lines.[9] These spectral signatures reflect cool, extended atmospheres conducive to molecule formation. In evolutionary terms, semiregular variables are closely associated with the asymptotic giant branch (AGB) phase of stellar evolution, where stars undergo significant mass loss that forms circumstellar dust envelopes, often detectable through infrared excess or radial velocity variations.[8] Some reside on the red giant branch (RGB) or in post-AGB stages, contributing to their observed irregularity as they transition toward planetary nebula formation.[6]Classification
Subtypes
Semiregular variable stars are classified into subtypes primarily based on their spectral types, pulsation periods, light amplitudes, and the degree of regularity in their light curves, as standardized in the General Catalogue of Variable Stars (GCVS).[10] These subtypes distinguish variations in stability and physical characteristics among giants and supergiants exhibiting semiregular behavior. The SRa subtype consists of late-type giants with spectral classes M, C, or S (or their emission-line variants Me, Ce, Se), featuring persistent single or multiple periodicities, with amplitudes and light-curve shapes that generally vary, periods ranging from 35 to 1200 days and visual amplitudes less than 2.5 magnitudes.[10] In contrast, SRb variables are also late-type giants of similar spectral classes but display poorly defined periods or alternating intervals of periodic and irregular variations, with periods from 20 to 2300 days and possible episodes of near-constancy.[10] SRc subtypes are characterized by late-type supergiants (M, C, S or Me, Ce, Se) with amplitudes around 1 magnitude in the visual band and periods from 30 days to several thousand days.[10] SRd variables encompass giants or supergiants of earlier spectral types F, G, or K (occasionally with emission lines), with periods between 30 and 1100 days and amplitudes ranging from 0.1 to 4 magnitudes in the visual.[10] Additionally, the SRs subtype includes short-period semiregular red giants, often pulsating in high overtones with periods of days to about a month. The SRs subtype was introduced in later updates to the GCVS (Name-Lists 67-77 and vol. V).[10]Relation to Other Variable Stars
Semiregular variable stars share significant similarities with Mira variables, as both classes consist of long-period pulsating red giants and supergiants on the asymptotic giant branch (AGB) of stellar evolution.[8] Unlike Miras, however, semiregulars exhibit smaller photometric amplitudes, typically less than 2.5 magnitudes in the visual band, and their periods are less strictly regular, often showing multi-periodic or quasi-periodic behavior.[10] This distinction arises from the underlying pulsation modes, where Miras predominantly pulsate in the fundamental mode with high regularity, while semiregulars display a mix of radial and non-radial modes leading to more variable light curves.[11] In contrast to irregular variables such as the Lb subtype, semiregulars demonstrate detectable periodicity in their light variations, albeit with some irregularity in amplitude and timing.[10] Lb variables, characterized by slow, non-periodic fluctuations in late-type giants without discernible cycles, often represent insufficiently observed stars that may later reveal semiregular patterns upon extended monitoring.[12] The boundary between these classes is thus somewhat fluid, with many initially classified Lb objects reclassified as semiregular after period analysis confirms underlying pulsations. Semiregular variables of the SRd subtype show overlaps with RV Tauri stars in spectral types, both featuring F to K supergiants with pulsational variability.[14] However, SRd stars differ in their period-amplitude behavior, displaying semiregular pulsations with periods from 30 to 1000 days and amplitudes under 2 magnitudes, whereas RV Tauri stars exhibit characteristic alternating deep and shallow minima on shorter cycles of 30 to 150 days due to binarity and dust effects.[10] This spectral overlap suggests possible evolutionary connections in post-AGB phases, though their light curve morphologies remain distinct.[15] Some semiregular variables exhibit overlaps with symbiotic stars, where the cool giant component undergoes pulsational variability akin to semiregular behavior.[16] In these systems, the primary variability stems from the pulsations of the red giant, with additional photometric changes from accretion onto a hot companion, but the semiregular pulsations dominate the long-term light curve.[17] Such overlaps highlight how pulsational instability in AGB stars can coexist with binary interactions without altering the core classification.[18] Evolutionarily, late-type semiregular variables (SRa, SRb, SRc) serve as an intermediate stage in the AGB evolution of low- to intermediate-mass stars, between earlier red giant branch phases and the more evolved, higher-amplitude Mira variables, reflecting increasing envelope instability and mass loss. SRd variables may relate to different evolutionary stages, potentially post-AGB or in higher-mass progenitors.[8] As AGB stars progress through thermal pulses, semiregular pulsations may transition to the more regular Mira phase.[19] This positioning underscores their role in tracing late-stage stellar evolution.[20]Pulsation Mechanisms
Physical Processes
Semiregular variable stars exhibit variability primarily through radial pulsations in their extended envelopes, akin to those in Mira variables but typically involving higher overtones or multiple modes rather than the fundamental mode alone.[21] These pulsations cause periodic expansions and contractions of the stellar surface, leading to luminosity changes as the radius and temperature vary. In asymptotic giant branch (AGB) stars, which comprise most semiregular variables, the envelopes are convective and loosely bound, facilitating these oscillations with periods ranging from tens to hundreds of days.[22] The driving force behind these pulsations is the kappa mechanism, operating in the ionization zones of helium and hydrogen within the envelope. During compression, rising temperatures in these partial ionization regions increase opacity (κ), trapping heat and causing further expansion; upon cooling, opacity decreases, releasing energy efficiently.[23] This cyclic modulation of radiative transfer creates a net energy gain for the pulsation, sustaining the instability despite the convective nature of AGB envelopes.[24] Multi-periodicity arises from the superposition of the fundamental mode and higher overtones, resulting in the characteristic semi-regular light curves that lack strict periodicity. Recent 3D radiation hydrodynamics simulations reveal that both radial and non-radial modes can be excited, leading to complex interactions. Observations indicate that most semiregular variables display two or more dominant periods, with ratios suggesting excitation of first and higher overtones rather than solely fundamental and first-overtone combinations. This mode interference produces irregular but quasi-periodic variations, as the amplitudes and phases of individual modes evolve over time. Additionally, stochastic processes and chaotic dynamics can contribute to the observed irregularity, particularly in less stable pulsators, as recent models show a transition from stochastic driving in smaller-amplitude variables to self-excited pulsations in semiregulars.[25] A subset of semiregular variables also exhibit long secondary periods (LSPs), approximately 10 times longer than the primary pulsation period, whose origins remain debated. Possible explanations include binary motion, where a companion induces radial velocity variations and circumstellar obscuration, or dynamical processes in the stellar envelope, such as radial pulsations in the outer layers or non-radial gravity modes.[26][27] Pulsations in semiregular variables enhance mass loss by levitating the envelope and enabling dust-driven winds, where radiation pressure on newly formed dust grains accelerates outflows. This process becomes prominent when pulsation periods exceed about 60 days, increasing mass-loss rates by factors of up to 10 and producing observable infrared excesses from reprocessed stellar light by circumstellar dust. In pulsation theory, the period approximates the dynamical timescale, scaling as , where is the stellar radius and is the sound speed (assumed roughly constant). For AGB stars with similar effective temperatures, luminosity , so and thus . This yields the approximate period-luminosity relation , modulated by envelope density variations.[23][28]Periods and Amplitudes
Semiregular variable stars exhibit primary pulsation periods typically ranging from 20 to over 2000 days, though most fall between 30 and 1200 days depending on subtype.[10] These stars often display multi-periodic behavior, with a dominant short primary period accompanied by a longer secondary period that can be approximately ten times the primary, contributing to their semi-regular variability.[29] Such multi-periodicity arises from the excitation of multiple pulsation modes, complicating the identification of individual cycles.[30] Amplitude variations in these stars are generally small, ranging from several hundredths of a magnitude up to 2.5 magnitudes for the more stable SRa subtype, while SRd variables can reach up to 4 magnitudes.[10] Factors influencing these variations include interference between pulsation modes, leading to episodes of reduced or enhanced amplitude over time.[30] Light curves typically show quasi-sinusoidal shapes for more regular pulsations or irregular, sawtooth-like forms during unstable phases, which are analyzed using Fourier decomposition to extract dominant periods and harmonics.[30] The inherent irregularity of semiregular variables necessitates long-term photometric monitoring to resolve periods accurately, as short-term observations often fail to capture multi-periodic trends or amplitude drifts. Surveys such as the All Sky Automated Survey (ASAS) and Gaia provide essential datasets spanning years to decades for this purpose.[31][32] Longer periods in these stars correlate with increased luminosity and stellar radius, as described by the pulsation period-mean density relation, where the approximate envelope pulsation timescale is given bywith as the radius, the gravitational constant, and the mass, linking observable variability to underlying stellar structure.[33]
Historical Context
Discovery and Early Studies
The recognition of semiregular variable stars emerged in the early 20th century as astronomers cataloged irregular brightness variations among red giant and supergiant stars, distinguishing them from more predictable Mira variables. At Harvard Observatory, Edward C. Pickering and Annie Jump Cannon played pivotal roles in identifying numerous such objects through systematic photographic surveys. Their efforts culminated in the Second Catalogue of Variable Stars, published in 1907, which documented over 1,000 variables, including many late-type stars exhibiting quasi-periodic fluctuations without the strict regularity of classical pulsators.[34] These early catalogs laid the groundwork for recognizing patterns in long-period variables, though semiregular behavior was initially described as "semi-regular" due to its Mira-like yet inconsistent nature.[35] In the 1920s and 1930s, detailed period analyses further highlighted the multi-periodic characteristics of these stars. This work built on earlier surveys, emphasizing the complexity of red variables beyond simple sinusoidal variations. Cecilia Payne-Gaposchkin advanced these studies in her 1930 publication The Stars of High Luminosity, where she analyzed high-luminosity red variables.[36] Her comprehensive surveys in the 1930s, detailed in Variable Stars (1938) co-authored with Sergei Gaposchkin, explicitly categorized semi-regular variables based on photographic light curves, attributing their behavior to intrinsic instabilities in evolved stars.[37] Prior to formal International Astronomical Union (IAU) classifications in the mid-20th century, semiregular variables were broadly grouped with long-period variables, lacking a separate designation but recognized for their shared spectral types (M, C, or S) and evolutionary stages as asymptotic giant branch stars. Early observers noted their quasi-periodic changes through visual and photographic means, but confirmation of these patterns awaited technological improvements. In the 1940s, the advent of photoelectric photometry, pioneered by Joel Stebbins, provided precise measurements that verified the semi-regular variations, revealing subtle amplitude modulations and period overlaps with accuracies down to 0.01 magnitudes—far surpassing earlier methods.[38] This technique, applied to select red variables, solidified the observational foundation for semiregular stars as a transitional class between regular pulsators and irregulars.Development of Classification
The formal classification of semiregular (SR) variable stars as a distinct category was adopted by the International Astronomical Union (IAU) during its 10th General Assembly in 1958, where it was defined as giants or supergiants showing fairly regular periodicity but with more irregularity than classical Cepheids or long-period variables like Miras, thereby distinguishing them from purely irregular variables. The initial subtypes, including SRc for late-type supergiants, were established at this time. Subsequent refinements to the SR classification were driven by updates to the General Catalogue of Variable Stars (GCVS), with Nikolai N. Samus and Elena V. Kazarovets leading efforts from the 1980s onward at the Sternberg Astronomical Institute; these updates incorporated new photometric data to refine subtypes and expand the catalog, ensuring ongoing maintenance through periodic revisions that reflect improved observational evidence.[39][40] In the 1990s, the SRd subtype was added to account for earlier spectral types (F, G, K) among yellow semiregular variables, based on detailed photometric analyses that highlighted their distinct pulsation behaviors.[41] Space-based surveys like Hipparcos in the 1990s provided precise parallaxes and period-luminosity relations for nearby SR variables, confirming multi-mode pulsations and enabling better statistical characterization of their distributions. Similarly, the Optical Gravitational Lensing Experiment (OGLE) surveys from the late 1990s onward delivered extensive light curves for extragalactic SR variables, yielding robust period statistics that reinforced the multi-periodic nature of the class.[42][43] In the 2000s, classifications evolved to incorporate long secondary periods (LSPs)—typically 5–10 times longer than primary pulsation periods—observed in many SR variables, addressing previous gaps in understanding their apparent irregularity through dedicated studies of light curve complexities.Examples
Bright Examples
One prominent example of a semiregular variable star visible to the naked eye is η Geminorum (also known as Propus), classified as subtype SRa. This M-type giant exhibits pulsations with a primary period of approximately 234 days and a visual amplitude of about 0.6 magnitudes, ranging from magnitude 3.3 to 3.9.[44] It was among the earliest stars recognized as semiregular variables, with variability first noted in systematic observations during the mid-19th century.[45] Located about 350 light-years away in the constellation Gemini, η Geminorum is easily observable under clear skies, contributing to its value for amateur astronomers monitoring long-period changes.[46] Antares (α Scorpii), classified as SRc, is a red supergiant with a primary period of about 1,300 days and visual amplitudes up to 1.5 magnitudes. Located approximately 550 light-years away, it occupies the upper red giant branch and is one of the brightest stars in Scorpius. Another well-known bright semiregular variable is Betelgeuse (α Orionis), an SRc subtype red supergiant with a dominant pulsation period near 400 days and visual amplitudes reaching up to 1.5 magnitudes, typically varying between magnitudes 0.0 and 1.6.[47] This star gained widespread attention for its unusual dimming event from late 2019 to early 2020, when it faded to magnitude 1.6 due to a massive dust ejection from its surface that formed an obscuring cloud.[48] As one of the brightest stars in the night sky at around 640 light-years distance, Betelgeuse marks the shoulder of the hunter in the constellation Orion and holds cultural significance in ancient traditions worldwide, symbolizing seasonal cycles and celestial hunters.[49] Its visibility from most latitudes makes it a staple for naked-eye observations of variability. The hypergiant μ Cephei, classified as SRc, displays erratic semiregular pulsations with a long primary period of about 730 days and a visual amplitude of roughly 1.7 magnitudes, fluctuating between magnitudes 3.4 and 5.1.[50] This M2Ia spectral type star, located approximately 5,600 light-years away, experiences significant mass loss at a rate of around 5 × 10^{-7} solar masses per year, forming an extensive circumstellar dust envelope.[51] Known as Herschel's "Garnet Star" for its vivid red hue, μ Cephei is intermittently visible to the naked eye from dark sites, particularly at maximum brightness, and serves as a benchmark for studying late-stage stellar evolution.[52] A closer example is L2 Puppis, an SRa subtype asymptotic giant branch star with a stable pulsation period of about 140 days and visual amplitudes up to 2 magnitudes, varying from magnitude 2.6 to 6.2.[53] At a distance of roughly 64 parsecs (209 light-years), its circumstellar envelope has been resolved through high-resolution imaging, revealing a dust disk indicative of ongoing mass ejection and potential binary interaction.[54] Positioned in the constellation Puppis between the brilliant stars Canopus and Sirius, L2 Puppis is intermittently naked-eye visible, offering opportunities to track its brightness cycles amid southern skies.[55]Other Notable Objects
RR Coronae Borealis (RR CrB) exemplifies the SRb subtype of semiregular variables, characterized by poorly defined periodicity in late-type giants. This M5 spectral type star exhibits a primary pulsation period of approximately 61 days with an amplitude of about 0.5 magnitudes, alongside a secondary period of around 377 days and amplitude of 0.6 magnitudes.[56] Its light variations, ranging from visual magnitude 8.4 to 10.1, provide insights into the irregular pulsation modes typical of oxygen-rich giants, as documented in early photometric surveys.[57] ρ Cassiopeiae (ρ Cas), classified as SRd, represents a rare yellow hypergiant with multiperiodic behavior, featuring a dominant long period of 820 days and amplitude near 2 magnitudes, causing brightness fluctuations from 4.1 to 6.2.[58] Its spectral type varies between F8Ia-0 and M3 during cycles, reflecting unstable atmospheric dynamics in evolved massive stars. Notable for explosive mass-loss events, ρ Cas underwent a significant outburst in 2000–2001, dimming by over 1 magnitude while its effective temperature dropped dramatically, ejecting material at high velocities and offering a window into pre-supernova evolution.[59] S Vulpeculae (S Vul), an SRd example of an F-type semiregular variable, displays a period of about 68 days with relatively stable light curve features, though its classification has been debated between semiregular and classical Cepheid types. Associated with stellar clusters such as Vul OB2, it serves as a key case for studying pulsations in intermediate-mass giants within clustered environments, where its position aids in calibrating period-luminosity relations for nearby populations. AU Arietis (AU Ari), the prototype for the SRS subtype, is a short-period semiregular red giant with a pulsation cycle of roughly 6 days and small amplitude of 0.1 magnitudes, ranging from 8.44 to 8.55 in visual light.[60] As an M0 star, it exemplifies high-overtone pulsators among red giants in clusters, facilitating research on the onset of pulsations in low-mass evolved stars near the tip of the red giant branch.[61] These objects hold substantial research value beyond their moderate brightness, enabling detailed investigations into long secondary periods (LSPs) that modulate primary pulsations by factors of 10 or more, potentially driven by binary interactions or large-scale convection. Spectroscopic and photometric monitoring reveals binary companions in some cases, influencing mass transfer and envelope dynamics.[26] Additionally, high-resolution observations, such as those with ALMA, have resolved circumstellar envelopes around semiregular variables, mapping dust and molecular distributions to quantify mass-loss rates and asymmetric outflows.[62]References
- https://arxiv.org/pdf/0902.4096