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Beta Canis Majoris
Beta Canis Majoris
Beta Canis Majoris
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Beta Canis Majoris
Location of β Canis Majoris (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Canis Major
Right ascension 06h 22m 41.98535s[1]
Declination −17° 57′ 21.3073″[1]
Apparent magnitude (V) 1.985[2] (1.97 – 2.01[3])
Characteristics
Spectral type B1 II-III[4]
U−B color index −0.99[2]
B−V color index −0.235[2]
Variable type β Cep[5]
Astrometry
Radial velocity (Rv)+33.7[6] km/s
Proper motion (μ) RA: −3.23 mas/yr[1]
Dec.: −0.78 mas/yr[1]
Parallax (π)6.62±0.22 mas[1]
Distance490 ± 20 ly
(151 ± 5 pc)
Absolute magnitude (MV)−3.93±0.04[7]
Details
Mass13±1[7] M☉
Radius8.44±0.56[7] R☉
Luminosity25,700+3,800
−3,300[7] L☉
Surface gravity (log g)3.70±0.08[7] cgs
Temperature25,180±1,120[7] K
Metallicity [Fe/H]0.04±0.10[8] dex
Rotation13.6±1.2[9] days
Rotational velocity (v sin i)31±5[8] km/s
Age12.2 or 13.8[9] Myr
Other designations
Mirzam, Murzim, Mirza[10], β Canis Majoris, 2 Canis Majoris, BD−17°1467, FK5 243, GC 8223, HD 44743, HIP 30324, HR 2294, SAO 151428, CCDM 06227-1757[11]
Database references
SIMBADdata

Beta Canis Majoris is a star in the southern constellation of Canis Major, the "Great Dog". Its name is a Bayer designation; it has the proper name Mirzam, pronounced /ˈmɜːrzəm/.[12] Visible to the naked eye, this is a variable star that ranges in apparent visual magnitude from 1.97 to 2.01 over a period of six hours.[3] Based on parallax measurements, it is located at a distance of about 500 light-years (150 parsecs) from the Earth.[1] The star is drifting further away from the Sun with a line of sight velocity of +34 km/s.[6] In the modern constellation it lies at the position of the dog's front leg.

Nomenclature

[edit]

Beta Canis Majoris is the star's Bayer designation, which is Latinized from β Canis Majoris and abbreviated Beta CMa or β CMa. The traditional names Mirzam, Al-Murzim or Murzim,[10] derive from the Arabic (مرزم) for 'The Herald', and probably refer to its position, heralding (i.e., rising before) Sirius in the night sky. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[13] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[14] included a table of the first two batches of names approved by the WGSN; which included Mirzam for this star.

In Chinese, 軍市 (Jūn Shì), meaning 'Market for Soldiers', refers to an asterism consisting of β Canis Majoris, Nu3 Canis Majoris, 15 Canis Majoris, Pi Canis Majoris, Omicron1 Canis Majoris and Xi1 Canis Majoris.[15] Consequently, β Canis Majoris itself is known as 軍市一 (Jūn Shì yī, English: the First Star of Market for Soldiers).[16] From this Chinese name arose the name Kuen She.[10]

The Dunhuang Star Chart noted β Canis Majoris as Yeji "Pheasant Cock", though was located about 10 degrees too far north of its correct position.[17]

Beta Canis Majoris was called Oupo by the people of the Tuamotus.[18]

Properties

[edit]
Pulsation cycles[8]
Frequency
(day−1) 		Amplitude
(km s−1)
3.9793 2.7
3.9995 2.6
4.1832 0.7

Mirzam is a Beta Cephei variable that varies in apparent magnitude between +1.97 and +2.01 over a six-hour period, a change in brightness that is too small to be discerned with the naked eye. It exhibits this variation in luminosity because of periodic pulsations in its outer envelope, which follow a complex pattern with three different cycles, all about six hours in length. The two dominant pulsation frequencies have a combined beat period of roughly 50 days. The strongest pulsation mode is a radial first overtone, while the second is non-radial.[8]

A light curve for Beta Canis Majoris, plotted from Hipparcos data[19]

This star has a mass of about 12–13 times the mass of the Sun with 7.4 or 8.2 times the Sun's radius.[9] The effective temperature of the star's outer envelope is about 24,700 K,[20] which is much higher than the Sun's at 5,778 K. The energy emitted at the high temperature of the former is what gives this star a blue-white hue characteristic of a B-type star.[21] The estimated age of Mirzam is 12–14 million years,[9] which is long enough for a star of this mass to have evolved into a giant star. The stellar classification of B1 II-III[4] indicates that the spectrum matches a star part way between a giant star and a bright giant. This star has a rotation period of 13.6 days and is inclined 57.6 ° as seen from Earth.[9]

Beta Canis Majoris is located near the far end of the Local Bubble,[22] a cavity in the local interstellar medium through which the Sun is traveling. It is located within the Mirzam Tunnel, a region of less dense concentration between the stars and HII regions surrounding the Ori OB1 and Vel OB2 associations. Beta Canis Majoris was the brightest star in the night sky around four million years ago, peaking with an apparent magnitude of −3.65, or more than seven times as bright as Sirius today.[23]

In culture

[edit]

Mirzam appears on the flag of Brazil, symbolising the state of Amapá.[24]

Murzim (AK-95) was a United States Navy Crater class cargo ship named after one of the star's alternative traditional names.

References

[edit]
Revisions and contributorsEdit on WikipediaRead on Wikipedia

Beta Canis Majoris

View on Grokipedia
from Grokipedia
Beta Canis Majoris (β CMa), also known as Mirzam, is a massive, hot bright giant star and pulsating variable of the Beta Cephei type located in the constellation . It has an apparent visual magnitude of 1.97 that varies slightly by about 0.04 magnitudes over periods near 6 hours due to non-radial pulsations, ranking it as the second-brightest star in its constellation after Sirius and visible to the from latitudes between +40° and -75°. The star lies at a distance of approximately 151 parsecs (492 light-years) from the Sun, based on its measurement of 6.62 ± 0.22 mas. Classified spectrally as B1II-III, Beta Canis Majoris exhibits the characteristics of a young, evolved massive star with an of about 25,000 K, enabling it to emit intense radiation that influences nearby interstellar clouds. Asteroseismic of its multiperiodic pulsations—primarily a radial mode at 3.9995 cycles per day and two quadrupolar modes—reveals a of 13 ± 1 solar masses, a radius of 8.4 ± 0.6 solar radii, a of approximately 26,000 solar luminosities, and an age of about 12 million years. These properties, derived from high-resolution and evolutionary modeling, highlight its role as a for studying convective core overshooting and internal mixing in early B-type stars. The star also appears as a visual double, with a faint magnitude-9.8 companion separated by 186 arcseconds, though no orbital connection is confirmed.

Nomenclature

Bayer Designation and Catalog Entries

Beta Canis Majoris, commonly abbreviated as β CMa, is the assigned to the star, following the system introduced by in his 1603 star atlas Uranometria, where Greek letters denote stars in order of brightness within each constellation. This designation marks it as the second star in the constellation , after α CMa (Sirius), though due to the variable nature of its brightness and the presence of other prominent stars like ε CMa (Adhara), it ranks as the fourth brightest in the constellation with an varying around 1.98. The Flamsteed designation for the star is 2 Canis Majoris, as cataloged by in his Historia Coelestis Britannica (1725), numbering stars sequentially by within each constellation. The precise equatorial coordinates of Beta Canis Majoris in the J2000.0 epoch are 06ʰ 22ᵐ 41.985ˢ and −17° 57′ 21.307″, based on high-precision astrometric measurements from the satellite and subsequent refinements.
CatalogDesignationReference
Henry Draper CatalogueHD 44743
Bright Star CatalogueHR 2294
Smithsonian Astrophysical ObservatorySAO 151428
General Catalogue of StarsGC 8223
As a pulsating variable star of the Beta Cephei type, it is included in variable star catalogues under the identifier β CMa. The proper name Mirzam for this star was officially approved by the International Astronomical Union's Working Group on Star Names on July 20, 2016.

Proper Names and Etymology

Beta Canis Majoris is most commonly known by its proper name Mirzam, derived from the Arabic term al-murzim, meaning "the herald" or "the announcer," a reference to the star's position as it rises shortly before the brighter Sirius in the constellation. Alternative Arabic forms include Al-Murzim and Murzim. The International Astronomical Union (IAU) standardized "Mirzam" as the proper name for the star through its Working Group on Star Names (WGSN) on July 20, 2016. In , the star is designated 軍市一 (Jūn Shì yī), the "First Star of the Market for Soldiers," as part of an asterism representing a military marketplace. On the ancient , dating to the (circa 649–684 CE), Beta Canis Majoris appears as Yeji, meaning "Pheasant Cock," depicted with a surrounding crown of 11 fainter stars forming part of the Jūnshì asterism, though positioned slightly inaccurately about 10° too far north. In the Tuamotuan tradition of the Tuamotu Archipelago, the star bears the name Oupo. This , β Canis Majoris, serves as the basis for its modern scientific usage alongside these traditional names.

Observational History

Discovery and Early Observations

Beta Canis Majoris, with an apparent visual magnitude of around 2.0, has been visible to the since ancient times as one of the brighter stars in the constellation , forming part of the celestial "Greater Dog" visible prominently in the winter sky for northern observers. The star was first cataloged by the ancient Greek astronomer Claudius Ptolemy in his during the 2nd century CE, where it appears as the second star in , described as "the star on the back" of the dog, positioned near the brilliant Sirius. In the , Danish included Beta Canis Majoris in his comprehensive star catalog, recording its position relative to Sirius as part of his precise naked-eye observations that improved upon Ptolemy's coordinates and laid the groundwork for later astronomy. During the 19th century, spectroscopic observations confirmed Beta Canis Majoris as a hot blue star; Italian Angelo Secchi classified it among his Type I spectra in the 1860s, characterized by strong lines typical of early-type stars, with subsequent refinements assigning it an early B spectral type around B2 by the 1880s. The star was included in Friedrich Wilhelm Argelander's Bonner Durchmusterung (1859–1862), cataloged as BD−17°1467, as one of the bright southern stars down to ninth magnitude, contributing to the systematic mapping of the sky for positional astronomy. Its variability was recognized in the early , leading to its classification as the prototype of the Beta Canis Majoris-type pulsating stars.

Classification as a Variable Star

The variability of was first recognized in 1908 through measurements that revealed periodic changes, initially suggesting a spectroscopic binary but later interpreted as pulsations. These early spectroscopic observations, conducted at the Lick Observatory, established the star's short-period behavior with a dominant cycle close to six hours. Photometric confirmation of the light variations followed in , with visual and photographic observations demonstrating consistent short-period pulsations aligned with the spectroscopic data. Early spectra from this era classified the star as spectral type B1 II-III, supporting its placement among massive main-sequence or B stars prone to pulsations. By the 1950s, as more members of the class were identified, Beta Canis Majoris was designated the prototype for the Beta Cephei variables (also termed β CMa stars), named after its characteristic short-period oscillations typical of early B-type stars near the main-sequence turnoff. This classification highlighted its role in defining the group, with the General Catalogue of Variable Stars designating it as β CMa. Further measurements in the confirmed the presence of multiple pulsation modes, indicating non-radial as well as radial components contributing to the observed variations. These findings solidified its status as a multiperiodic pulsator, distinguishing it within the prototype class.

Physical Properties

Position and Visibility

Beta Canis Majoris is located in the constellation at equatorial coordinates of 06ʰ 22ᵐ 41.985ˢ and −17° 57′ 21.31″ (J2000 ). Its galactic coordinates are longitude 226.06° and latitude −14.27°. Based on parallax measurements from the mission and refined with data, the star lies at a distance of approximately 490 light-years (151 parsecs) from the Solar System. With an apparent visual magnitude of 1.985, varying slightly between 1.97 and 2.01 due to its pulsations, Beta Canis Majoris ranks as the second-brightest in after Sirius. This brightness makes it easily visible to the under clear skies. The is best observed from mid-northern latitudes during , when reaches its highest point in the evening sky, achieving altitudes up to about 73° at the but lower toward the north (e.g., around 50° at 40° N ). Known historically as Mirzam ("the announcer"), it rises shortly before Sirius, serving as a celestial herald in the winter sky for northern observers. From southern hemisphere locations south of about 17° S, it remains visible for much of the year without setting, though not truly circumpolar except near the .

Stellar Characteristics

Beta Canis Majoris is classified as a B1 II-III , indicating a blue-white giant or bright giant with a spectrum dominated by strong lines and a luminosity class between giant and bright giant. This spectral type reflects its high surface temperature and advanced evolutionary state, where the has left the and expanded due to core hydrogen exhaustion. The has a mass of 13 ± 1 solar masses (M⊙), determined through a combination of gravitational mass estimates from orbital dynamics and evolutionary models consistent with its position in the Hertzsprung-Russell diagram. Its radius measures 8.44 ± 0.56 solar radii (R⊙), derived from interferometric angular diameter measurements combined with the parallax distance of approximately 151 parsecs. The is 25,700^{+3,800}_{-3,300} L⊙, calculated from the bolometric flux and angular size using non-local atmosphere models. The is 25,180 ± 1,120 K, supporting its blue-white appearance and high ionization levels in the stellar atmosphere. Surface gravity is log g = 3.70 ± 0.08 (in cgs units), indicative of a low-density envelope typical of post-main-sequence . is near-solar, as inferred from spectroscopic analysis of metal lines in the . Overall, Beta Canis Majoris is a post-main-sequence bright giant in the β Cephei , evolving toward the phase after core hydrogen burning, with an age of approximately 12-14 million years estimated from stellar isochrones.

Kinematics and Age

Beta Canis Majoris exhibits a of +33.7 ± 0.5 km/s, indicating it is receding from the Solar System. Its components are -3.23 ± 0.19 mas/yr in and -0.78 ± 0.20 mas/yr in , corresponding to a small tangential of approximately 2.4 km/s at its of 151 pc. These astrometric parameters yield space components relative to the local standard of rest of U = -20 km/s (towards the ), V = -10 km/s (in the direction of galactic rotation), and W = +15 km/s (towards the galactic north pole), consistent with a young massive field . The star rotates with an equatorial velocity of 31 ± 5 km/s and a rotational period of 13.6 ± 1.2 days, as determined from mode identification in its pulsation spectrum and spectroscopic analysis of line profiles. The projected rotational velocity v sin i is approximately 20 km/s, with an inclination angle of 56.7 ± 1.7° relative to the . These rotational properties suggest moderate spin for a massive B-type giant, influencing the observed line broadening in high-resolution spectra. Beta Canis Majoris has an estimated age of 12.4 ± 0.7 million years, derived from fitting tracks to its pulsation frequencies via asteroseismic modeling, including constraints from avoided crossings in the modes. This places it in the post-main-sequence phase for a of its (around 13 solar masses). Its kinematics are consistent with those of young OB stars but it is not a member of the OB1 association due to the association's expanded structure and velocity dispersion of several km/s. Around 4 million years ago, the reached its peak brightness as viewed from the Solar System.

Variability

Pulsation Modes and Periods

Beta Canis Majoris serves as the prototype for Beta Cephei variables, a subclass of massive B-type stars characterized by pulsations driven by the kappa mechanism operating in the ionization zone. This instability arises from opacity variations during the partial ionization of , leading to periodic compression and expansion of the stellar envelope. The star's variability was first noted in 1908 by Samuel Albrecht through measurements, cementing its role as the namesake for this class of pulsators. The pulsations exhibit multi-periodicity, dominated by three closely spaced modes that produce observable interference effects. The dominant mode has a period of approximately 6.00 hours (frequency 3.9995 cycles per day; radial, ℓ=0, m=0), while secondary modes are identified at ~6.03 hours (3.9793 cycles per day; quadrupolar, ℓ=2, m=2) and ~5.74 hours (4.1832 cycles per day; non-radial) through combined analysis of radial velocity curves and photometric data. These periods correspond to frequencies of 3.9793, 3.9995, and 4.1832 cycles per day, respectively, with the close proximity of the first two frequencies resulting in a beat period of about 50 days from mode interference. Radial velocity measurements reveal amplitudes of about 2.7 km/s for the dominant modes (2.6-2.7 km/s), reflecting surface motions. Asteroseismic studies identify the dominant pulsations as radial p-modes, with evidence of non-radial components in at least two modes, providing constraints on the star's internal structure and rotation.

Amplitude and Evolutionary Implications

The visual magnitude of Beta Canis Majoris varies between 1.97 and 2.01, corresponding to a total ΔV ≈ 0.04 mag, with the small-scale fluctuations arising from the superposition of multiple pulsation modes that cause irregular light variations. Photometric observations in the V-band reveal nearly sinusoidal light curves, which have been analyzed using Fourier transforms to decompose the signal into dominant frequencies with amplitudes on the order of 20–25 millimagnitudes for the primary mode and smaller contributions from secondary modes. These variations are subtle and require precise photometry to detect, as the overall brightness change is not discernible to the . Spectroscopic monitoring shows line-profile variations in the star's absorption lines, with amplitude and phase shifts across the profiles that confirm the presence of non-radial pulsation modes, including quadrupolar (ℓ=2) and radial (ℓ=0) components. Such non-radial modes contribute to the observed photometric irregularity by introducing asymmetric distortions in the light curve. Over longer timescales spanning decades, the pulsation amplitudes exhibit modulation, with some modes showing variable strengths that may indicate temporary mode switching or beating effects among closely spaced frequencies. The pulsations place Beta Canis Majoris within the on the Hertzsprung-Russell diagram, a region occupied by massive B-type stars nearing the end of core burning, where partial ionization zones drive radial and non-radial oscillations. Evolutionary models for B1 supergiants predict that such stars cross this instability strip during the exhaustion of core , experiencing a brief phase of enhanced pulsational activity before evolving toward the stage. Asteroseismic analysis of the pulsation periods provides constraints on the star's interior , yielding a of 13.5 ± 0.5 M_⊙, an age of 12.4 ± 0.7 Myr, and significant core overshooting of 0.20 ± 0.05 scale heights, which refines evolutionary models by accounting for mixing beyond the convective core during main-sequence hydrogen burning. These parameters align with the star's position in the and support the interpretation of its variability as a of advanced core evolution in a massive star.

Interstellar Environment

Location in the Local Bubble

Beta Canis Majoris is situated near the far end of the Local Bubble, a low-density cavity in the approximately 300 parsecs across, sculpted by multiple supernovae explosions over the past 10-15 million years. The star lies at a distance of approximately 492 light-years (151 parsecs) from the Sun, positioning it within this expansive void. This location places Beta Canis Majoris within the hypothesized Mirzam Tunnel, an extension of the Local Bubble extending toward the constellation, characterized by even lower gas densities and embedding the star in a sparse interstellar structure. Line-of-sight absorption studies toward the star reveal sparse neutral , with column densities indicating a neutral-free consistent with the hot, million-degree plasma filling the Bubble. As a B1 giant, Beta Canis Majoris contributes significantly to the local ultraviolet flux, alongside the nearby ε Canis Majoris, ionizing neutral gas in adjacent interstellar clouds such as the Local Interstellar Cloud complex. This ionization is detailed in recent modeling, which attributes much of the observed densities and temperatures in these clouds to the combined extreme- radiation from these stars. This isolation underscores its position in the diffuse, cavity-dominated environment of the Local Bubble's periphery.

Historical Proximity to the Solar System

Approximately 4.4 million years ago, Beta Canis Majoris passed within 10 ± 1 parsecs (about 33 light-years) of the Sun, marking its closest historical approach to the Solar System. This proximity was determined through backward integration of the star's and using high-precision astrometric data. At that time, the star's ionizing flux incident on the Solar System was 180–200 times greater than its current value, potentially fully ionizing local interstellar clouds. Due to its intrinsic and the reduced , Beta Canis Majoris would have appeared exceptionally bright in Earth's sky, brighter than Sirius appears today. This visual prominence occurred as the star moved along a from a more southerly galactic position toward its current location in the constellation , with its velocity vector (+33.7 km/s ) ensuring continued recession from the Sun. The star's passage may have contributed to the formation of low-density interstellar tunnels associated with the Local Bubble, possibly through its powerful stellar winds or in conjunction with nearby supernovae from the Scorpius-Centaurus OB association. Enhanced during this epoch could have influenced the state of the proto-Solar neighborhood, affecting the environment around the young Solar System. Recent simulations, incorporating updated astrometric measurements as of 2025, confirm this close encounter and its dynamical implications.

Cultural Significance

Mythological and Historical References

In , Beta Canis Majoris is incorporated into the constellation , representing one of Orion's loyal hunting dogs pursuing prey across the heavens. Ancient texts by , , and describe the constellation as the greater dog accompanying the hunter Orion, with Beta Canis Majoris positioned on the dog's foreleg. This placement earned the star a role as a herald, rising shortly before the brilliant Sirius to signal its approach in the night sky. In Arabic astronomy, the bore the name al-Murzim, translating to "the announcer" or "herald," due to its precedence in rising before Sirius, the preeminent "Dog Star" of the southern . Arab navigators relied on such prominent stars for orientation in the southern skies, where al-Murzim aided in charting courses across vast maritime expanses. The name's highlights this signaling function, bridging mythological and practical celestial observation. Chinese astronomers assigned Beta Canis Majoris to the Jūn Shì asterism, known as the "Market for Soldiers," a grouping evoking a bustling encampment where troops exchanged provisions amid military campaigns. This asterism, encompassing several stars in Canis Major, reflected broader themes of strategic gathering in traditional Chinese uranography. Among Polynesian cultures, Tuamotuan voyagers in the Pacific islands named the star Oupo and incorporated it into their wayfinding practices, using its consistent position relative to other stars to guide long-distance ocean travels across the archipelago. Historical astronomical records document Beta Canis Majoris within the constellation , as cataloged by in his second-century among the 48 ancient constellations. The star later appeared in tenth-century Arabic compilations, notably al-Sufi's , which integrated Ptolemaic positions with indigenous Arabic stellar nomenclature and illustrations of the Greater Dog.

Modern Usage and Symbolism

Beta Canis Majoris, known as Mirzam, is depicted on the as one of the stars in the representing the night sky over Rio de Janeiro, symbolizing the state of . The flag's design, which includes 27 stars for Brazil's federative units, was originally adopted on November 19, 1889, with updates to the stellar configuration in following the creation of new states, including Amapá in 1988. In naval history, the star served as the namesake for USS Murzim (AK-95), a Crater-class cargo ship of the U.S. Navy commissioned on May 14, 1943, during World War II. The vessel, originally laid down as SS Brigham Young, transported supplies across the Pacific and earned one battle star before decommissioning in 1946; its name derives from Mirzam as the second-brightest star in Canis Major. In contemporary astronomy, Beta Canis Majoris is recognized as the prototype for the Beta Cephei class of variable stars, characterized by short-period pulsations, and plays a central role in asteroseismology research probing stellar interiors through oscillation modes. Detailed spectroscopic studies over multiple years have identified multiple pulsation frequencies in the star, aiding models of massive B-type star evolution. It features prominently in outreach efforts by organizations like the American Association of Variable Star Observers, where it exemplifies beat phenomena from overlapping pulsation periods for amateur astronomers studying bright variables. The star's traditional name, Mirzam—meaning "the announcer" in —symbolizes its role in heralding the rise of Sirius, the brighter "Dog Star," a concept echoed in modern astronomy education to illustrate constellation lore and stellar visibility sequences. This heraldic imagery influences educational narratives on as a winter constellation, emphasizing how precursor stars like Mirzam guide observers to prominent night-sky features. In 2025 media, Beta Canis Majoris appears in astronomical observing guides highlighting winter sky events, such as monthly sky reports featuring Canis Major's bright stars for viewers during December through February.

References

  1. http://www.ianridpath.com/startales/canismajor.html
  2. https://simbad.u-strasbg.fr/simbad/sim-basic?Ident=bet+CMa
  3. https://www.aanda.org/articles/aa/abs/2006/44/aa4980-06/aa4980-06.html
  4. https://arxiv.org/abs/2508.03800
  5. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=bet+CMa
  6. https://www.pas.rochester.edu/~emamajek/WGSN/WGSN_bulletin1.pdf
  7. https://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Canis_Major*.html
  8. https://stars.astro.illinois.edu/sow/mirzam.html
  9. http://bonnetbidaud.free.fr/chine/articles/Bonnet-Bidaud_et_al_2009_JAHH_v12_n1_p39sm.pdf
  10. https://www.star-facts.com/mirzam/
  11. https://www.constellation-guide.com/constellation-list/canis-major-constellation/
  12. http://www.ianridpath.com/startales/almagest.html
  13. https://www.aanda.org/articles/aa/pdf/2010/08/aa14002-10.pdf
  14. https://adsabs.harvard.edu/full/1950PA.....58..153M
  15. https://heasarc.gsfc.nasa.gov/w3browse/all/bd.html
  16. https://adsabs.harvard.edu/full/1952AJ.....57..227W
  17. https://www.aanda.org/articles/aa/pdf/2006/44/aa4980-06.pdf
  18. https://adsabs.harvard.edu/full/1909PASP...21...84A
  19. https://academic.oup.com/mnras/article/161/3/257/2603321
  20. https://adsabs.harvard.edu/full/1962ZA.....56...27V
  21. http://simbad.cds.unistra.fr/simbad/sim-ref?bibcode=2007A%26A...474..653V
  22. http://simbad.cds.unistra.fr/simbad/sim-ref?bibcode=2002yCat.2237....0D
  23. https://earthsky.org/constellations/canis-major-the-greater-dog-sirius/
  24. https://arxiv.org/abs/astro-ph/0607261
  25. https://adsabs.harvard.edu/full/1967MNRAS.136...51B
  26. https://ui.adsabs.harvard.edu/abs/1973MNRAS.161..257S
  27. https://ui.adsabs.harvard.edu/abs/1978MNRAS.184..825S
  28. https://www.cosmos.esa.int/web/gaia/iow_20220112
  29. https://iopscience.iop.org/article/10.1086/324016/fulltext/
  30. https://theskylive.com/sky/stars/mirzam-beta-canis-majoris-star
  31. https://ntrs.nasa.gov/citations/19910053998
  32. https://adsabs.harvard.edu/full/1991ApJ...373..556W
  33. https://adsabs.harvard.edu/full/1998ASPC..143..290D
  34. https://webspace.science.uu.nl/~gent0113/alsufi/alsufi_constellations.htm
  35. https://crwflags.com/FOTW/FLAGs/br_astro.html
  36. https://www.history.navy.mil/research/histories/ship-histories/danfs/m/murzim.html
  37. https://ui.adsabs.harvard.edu/abs/2006A%26A...459..589M/abstract
  38. https://www.aavso.org/vsots_betacep
  39. https://www.skyatnightmagazine.com/advice/constellation-canis-major
  40. http://stars.astro.illinois.edu/sow/mirzam.html
  41. https://skyandtelescope.org/astronomy-news/observing-news/this-weeks-sky-at-a-glance-february-14-23/
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