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Messier 67
Messier 67
Messier 67
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Messier 67
Open cluster Messier 67 in Cancer
Observation data (J2000.0 epoch)
Right ascension08h 51.3m
Declination+11° 49′
Distance~2.61–2.93 kly (800–900 pc[1][2][3][4])
Apparent magnitude (V)6.1
Apparent dimensions (V)30.0′
Physical characteristics
Radius10 ly[citation needed]
Estimated age3.2 to 5 billion years
Other designationsNGC 2682, Cr 204
Associations
ConstellationCancer
See also: Open cluster, List of open clusters

Messier 67 (also known as M67 or NGC 2682) and sometimes called the King Cobra Cluster or the Golden Eye Cluster[5] is an open cluster in the southern, equatorial half of Cancer. It was discovered by Johann Gottfried Koehler in 1779. Estimates of its age range between 3.2 and 5 billion years. Distance estimates are likewise varied, but typically are 800–900 parsecs (2,600–2,900 ly).[1][2][3][4] Estimates of 855, 840, and 815 pc were established via binary star modelling and infrared color-magnitude diagram fitting.[2][3][4]

Description

[edit]

M67 is not the oldest known open cluster; several Milky Way clusters are known to be older, yet farther than M67. It is a paradigm study object in stellar evolution:[6]

  • it is well-populated
  • has negligible amounts of dust obscuration
  • all its stars are at the same distance and age, save for approximately 30 anomalous blue stragglers

M67 is one of the most-studied open clusters, yet estimates of its physical parameters such as age, mass, and number of stars of a given type, vary substantially. Richer et al. estimate its age to be 4 billion years, its mass to be 1080 solar masses (M☉), and number its white dwarfs at 150.[7] Hurley et al. estimate its current mass to be 1,400 M☉ and its initial mass to be approximately 10 times as great.[8]

It has more than 100 stars similar to the Sun, and numerous red giants. The total star count has been estimated at well over 500.[9] The ages and prevalence of Sun-like stars had led some astronomers to theorize it as the possible parent cluster of the Sun.[10] However, computer simulations disagree on whether the outer Solar System would have survived an ejection from M67,[11][12] and the cluster itself would probably not have survived such an ejection event.[13]

The cluster contains no main sequence stars bluer (hotter) than spectral type F, other than perhaps some of the blue stragglers, since the brighter stars of that age have already left the main sequence. In fact, when the stars of the cluster are plotted on the Hertzsprung-Russell diagram, there is a distinct "turn-off" representing the stars which have terminated hydrogen fusion in the core and are destined to become red giants. As a cluster ages, the turn-off moves progressively down the main sequence to cooler stars.

It appears that M67 has a bias toward heavier stars. One cause of this is mass segregation, the process by which lighter stars gain speed at the expense of more massive stars during close encounters, which moves them to greater average distance from the center of the cluster or allows escape altogether.[14]

A March 2016 joint AIP/JHU study by Barnes et al. on rotational periods of 20 Sun-like stars, measured by the effects of moving starspots on light curves, suggests that these approximately 4 billion-year old stars spin in about 26 days – like the Sun, which has a period at the equator of 25.38 days.[15] Measurements were carried out as part of the extended K2 mission of Kepler space telescope. This reinforces the applicability of many key properties of the Sun to stars of the same size and age, a fundamental principle of modern solar and stellar physics.[16] The authors abbreviate this as the "solar-stellar connection".[16]

Exoplanets

[edit]
Artistic impression of a exoplanet orbiting a star in Messier 67.

A radial velocity survey of M67 has found exoplanets around five stars in the cluster: YBP 1194, YBP 1514, YBP 401, Sand 978, and Sand 1429.[17][18][19][20] A sixth star, Sand 364, was also thought to have a planet, but a follow-up study did not find evidence for it and concluded that the radial velocity variations have a non-planetary origin, likely stellar variability.[21]

[edit]
  • Messier 67 (SDSS, optical and near-infrared)
    Messier 67 (SDSS, optical and near-infrared)
  • Hertzsprung-Russell diagram for two open clusters, M67 and NGC 188, showing color-magnitude data
    Hertzsprung-Russell diagram for two open clusters, M67 and NGC 188, showing color-magnitude data
  • Artist's impression video showing a hot Jupiter exoplanet orbiting close to a star in Messier 67
  • Artist's impression of a hot Jupiter exoplanet in the star cluster Messier 67
    Artist's impression of a hot Jupiter exoplanet in the star cluster Messier 67

See also

[edit]

References

[edit]
[edit]
Revisions and contributorsEdit on WikipediaRead on Wikipedia

Messier 67

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from Grokipedia
Messier 67 (M67; also known as NGC 2682) is an open star cluster located in the constellation Cancer, approximately 2,800 light-years from and about 1,500 light-years above the plane of the galaxy. It is one of the oldest known open clusters in the galaxy, with an age of around 4 billion years, comparable to the age of the Solar System, and contains over 500 gravitationally bound stars spanning various evolutionary stages, including main-sequence stars, red giants, white dwarfs, and blue stragglers. The cluster spans an of about 25 arcminutes on the sky, corresponding to a physical diameter of roughly 20 light-years, and has a solar-like ([Fe/H] ≈ 0.03). First recorded as a nebula by German astronomer Johann Gottfried Koehler in 1779 and independently identified as a star cluster by French astronomer in 1780—who added it as the 67th entry in his famous catalog of non-cometary objects—M67 has been a key target for astronomical study due to its advanced age and proximity. Its is 08h 51m 23.5s and +11° 48′ 54″ (J2000 ), with a systemic of about 34 km/s and proper motion components of -11 mas/yr in and -3 mas/yr in . Unlike younger open clusters concentrated near the , M67's elevated position makes it less affected by interstellar dust, allowing clearer observations of its stellar population. M67 is notable for its diverse stellar content, including approximately 30 stars—unusually hot and bright objects thought to form through in binary systems or stellar mergers—and several confirmed exoplanets orbiting member stars within the cluster, including two hot Jupiters around Sun-like stars and a warm Jupiter discovered in 2024, providing insights into planet formation in ancient environments. The cluster's population, with an average mass of 0.60 solar masses, serves as a "cosmic clock" for verifying models and determining the cluster's age. As one of the best-studied open clusters, M67 offers a benchmark for understanding the dynamical evolution of star clusters, binary interactions, and the chemical enrichment processes in the Milky Way's disk.

Discovery and Observation

Discovery

Messier 67 was first recorded as a distinct celestial object by the German astronomer Johann Gottfried Koehler before 1779, who described it as "a rather conspicuous in elongated figure, near Alpha of Cancer" using his limited instrumentation, which prevented him from resolving it into individual stars. The cluster was independently rediscovered by French astronomer on April 6, 1780, during his systematic search for comets, when he noted it as a "cluster of small stars with nebulosity, below the southern claw of Cancer," with its position determined relative to Alpha Cancri. This observation led to its formal inclusion as the 67th entry in Messier's renowned catalog of nebulae and star clusters, published in the Connaissance des Temps for 1781. In 1784, British astronomer observed Messier 67 using his 20-foot and described it as "a most beautiful cluster of ; not less than 200 in view," highlighting its stellar nature more clearly than prior accounts and contributing to early understandings of open clusters. The cluster received its designation as NGC 2682 from observations conducted by between 1826 and 1830, where he characterized it as a "pretty rich cluster of scattered between 10th and 15th magnitude," with estimates of up to 200 member filling the field of view.

Historical Observations

Following its initial cataloging by in 1780, Messier 67 became a subject of detailed telescopic scrutiny in the , particularly through the observations of . Using his 20-foot reflector during sweeps between 1826 and 1830, Herschel resolved the cluster into a "pretty rich cluster of scattered stars between 10th and 15th magnitude," estimating 100 to 200 stars that filled the field of view and noting its remarkable brightness and extent. His father, , had earlier described it in 1784 as a "most beautiful cluster of stars; not less than 200 in view" with his larger instrument, emphasizing its stellar richness over nebulous appearance. Other astronomers, such as William Smyth in 1836, reinforced these findings, portraying it as a "rich but loose cluster... consists principally of a mass of stars of the 9th and 10th magnitude, gathered somewhat in the form of a ." Advancements in during the late 19th and early 20th centuries allowed for the detection of fainter members beyond visual limits. The Observatory's extensive plate collection, initiated in the under Edward C. Pickering, captured images of Messier 67 that revealed dimmer down to 15th magnitude or fainter, enabling more complete membership assessments. These early dry-plate exposures, part of broader surveys, highlighted the cluster's sparse outer envelope and contributed to quantitative counts, distinguishing true members from field . Spectroscopic investigations in the early 20th century, led by as part of the Henry Draper Catalogue (published 1918–1924), classified the types of prominent in Messier 67. Cannon's , refining earlier schemes, identified dominant G- and K-type giants among the brighter members, with spectra showing strong absorption lines indicative of cooler, evolved . This work, based on Harvard's photographic spectra, provided the first systematic typing for dozens of cluster , revealing a paucity of hot O- and B-type objects. By the 1920s, analyses of color-magnitude data from these photographic plates led to the recognition of Messier 67 as an old . Harlow Shapley's studies, including photoelectric and photographic photometry published in 1917 and 1919, constructed early color indices for Messier 67 stars, showing a main sequence turnoff at cooler temperatures and an elevated giant branch compared to younger clusters like the . This morphology, lacking blue giants and featuring red giants, indicated an age of several billion years, positioning it as a key example of galactic cluster evolution akin to the Hyades but older.

Modern Studies

In the mid-20th century, the development of photoelectric photometry enabled the construction of detailed color-magnitude diagrams (CMDs) for Messier 67 (M67), providing early quantitative insights into its advanced age and . A seminal study by Johnson and Sandage in 1955 derived the first such diagram from observations of over 100 stars, revealing a main-sequence turnoff indicative of an age exceeding 4 billion years and a populated by evolved stars, which highlighted M67's role as a benchmark for understanding effects on . This work confirmed M67 as one of the oldest known open clusters, with its CMD morphology suggesting minimal ongoing and significant dynamical relaxation. Advancements in space-based imaging during the 1990s further resolved faint stellar populations in M67, particularly through observations. Using the Wide Field Planetary Camera 2, Richer et al. in 1998 imaged the cluster's core to depths reaching V ≈ 28, clearly delineating the cooling sequence for the first time and identifying over 20 as brighter, hotter outliers on the CMD. These findings quantified the cluster's population, estimating a total of approximately 100 such remnants and supporting mass-transfer or collision scenarios for formation, while establishing M67's distance at around 900 parsecs based on the sequence's . The European Space Agency's mission, beginning with Data Release 2 in 2018, revolutionized membership determination and for M67 by providing precise s and parallaxes for thousands of stars across a wide field. Carrera et al. in 2019 analyzed DR2 data to select over 1,000 probable members up to 150 parsecs from the cluster center, revealing an extended halo twice the previously known size and refining the distance to 840 ± 40 parsecs through isochrone fitting. Subsequent releases, including DR3 in 2022, enhanced accuracy to below 0.1 mas yr⁻¹, enabling detailed dynamical modeling and confirmation of low-mass star retention, which underscores M67's evolutionary history without significant mass loss. Recent theoretical work has leveraged M67's well-characterized stellar parameters to probe uncertainties in models. A study by Byrom et al. compared four isochrone grids—DSEP, GARSTEC, , and YREC—applied to observed CMD positions of M67 main-sequence and giant stars, finding age discrepancies up to 20% across grids, particularly for red giants where YREC and yielded younger estimates (around 2.6 Gyr) than the cluster's accepted 4 Gyr value. This highlights sensitivities to convective overshoot and opacity treatments, advocating for hybrid models to better match empirical data from M67. In 2025, asteroseismology emerged as a powerful tool for probing M67's interiors, with Reyes et al. detecting solar-like acoustic oscillations (p-modes) in 27 evolved stars spanning subgiants to red giants using space- and ground-based photometry. The analysis revealed large frequency separations (Δν) decreasing from ~8 μHz in subgiants to ~4 μHz in giants, tracing a rapid deepening of convective envelopes that evolves the acoustic cavity depth by over 50% during this phase, consistent with models of envelope expansion but revealing unexpected plateaus in mode ratios. These detections, with individual mode frequencies resolved to ~0.1 μHz precision, provide direct constraints on convective zone , affirming M67's age at 4.0 ± 0.2 Gyr without reliance on surface parameters.

Physical Characteristics

Location and Visibility

Messier 67 resides in the constellation Cancer, positioned near the border with Hydra. Its equatorial coordinates in the J2000.0 epoch are 08h 51m 23s and +11° 48′ 54″. The cluster lies at a distance of approximately 850 parsecs (2,770 light-years) from , with recent refinements from DR3 data placing it at 834 ± 37 pc. With an apparent visual magnitude of 6.1, Messier 67 appears as a faint, fuzzy patch visible to the under dark skies, though or a small reveal it more clearly as a loose grouping of stars. The cluster spans an apparent of approximately 25–30 arcminutes across the , comparable to the full Moon's diameter, allowing observers to discern its extent even in modest instruments. From northern latitudes, Messier 67 is best observed between March and June, when the constellation Cancer rises high in the evening sky amid its notably faint stars. During this period, the cluster's position facilitates optimal visibility, free from significant atmospheric interference near the zenith.

Structure and Dimensions

Messier 67 exhibits a compact structure typical of old open clusters, with a core radius of approximately 1.1 parsecs and a tidal radius of about 8.4 parsecs, delineating the spatial extent beyond which stars are more likely to escape due to galactic tidal forces. The overall physical radius of the cluster, encompassing the main body of member stars, spans roughly 7 to 10 light-years (approximately 2 to 3 parsecs), corresponding to the half-mass or half-light radius where half the cluster's stellar mass or light is contained. Recent Gaia data reveal an extended halo reaching up to 50 parsecs, suggesting ongoing dynamical evolution and possible tidal interactions, though the core remains well-defined. The total mass of the cluster is estimated at 1 to 2 × 10³ solar masses, distributed among approximately 500 confirmed member stars within the half-light radius, with observations identifying up to 800 probable members overall. This supports the cluster's gravitational binding against dissolution over its age of several billion years. The stellar profile follows a model with a concentration c ≈ 0.9, indicating moderate central concentration where decreases from a high core value of several stars per cubic to negligible levels at the tidal boundary. Interstellar dust within the cluster is negligible, with low reddening (E(B-V) ≈ 0.04 mag) enabling unobscured views of its stellar content across the . This transparency facilitates detailed studies of the cluster's morphology, revealing no significant obscuration in the .

Age and Metallicity

Messier 67 is an old with an age estimated at 3.2–4.5 billion years, primarily determined through isochrone fitting to the color-magnitude diagram, focusing on the main-sequence turnoff point where stars have exhausted their fuel. This method calibrates the cluster's evolutionary stage against theoretical stellar models such as and BaSTI, which account for parameters like and abundance to match observed stellar distributions. An independent age estimate comes from the cooling sequence, where the faintest white dwarfs provide a clock based on their post-main-sequence cooling times; for Messier 67, this yields a cooling age of approximately 4.3 billion years, consistent with the turnoff age of about 4.0 billion years. The cluster's is solar, with [Fe/H] = 0.0 ± 0.1, derived from high-resolution of member stars using instruments like VLT/FLAMES-UVES to measure iron and other elemental abundances relative to the Sun. Messier 67 formed in the galactic disk roughly 4 billion years ago and has persisted due to its dominance by low-mass stars, which resist dynamical disruption, and its position approximately 1,500 light-years above the plane, reducing interactions with dense interstellar material.

Member Stars and Types

Messier 67 contains approximately 500 probable member stars, as determined from astrometric data including s and parallaxes provided by the Data Release 3 (DR3). Membership in the cluster is primarily established through these criteria, which help distinguish cluster stars from foreground and background field stars within the cluster's spatial extent. The members span an apparent visual magnitude range of roughly 8 to 15, with over 200 stars brighter than V=15 magnitude contributing significantly to the cluster's observed stellar inventory. The stellar population of Messier 67 is dominated by main-sequence dwarfs of spectral types G and , resembling the Sun in composition and evolutionary stage, with about 100 such Sun-like stars identified. These G-K dwarfs form the bulk of the lower , reflecting the cluster's advanced age. The population also includes numerous red giants, primarily of K-type, with at least 11 bright examples exhibiting absolute magnitudes between +0.5 and +1.5. Among the evolved stars, Messier 67 hosts approximately 200 white dwarfs, consistent with predictions from single- and binary-star evolution models for a solar-metallicity cluster of this age. Additionally, approximately 30 blue stragglers are present, appearing brighter and bluer than the main-sequence turnoff due to processes such as binary or mergers. The binary fraction is notably high, reaching about 38% among main-sequence solar-type , indicating a significant role for binary systems in the cluster's dynamics and evolution.

Evolutionary Features

Messier 67 serves as a benchmark for understanding in an old , with its main-sequence turnoff occurring at approximately 1.2 solar masses, corresponding to an age of about 4 billion years. This turnoff point marks the stage where stars of that mass have exhausted their core fuel and begin evolving off the , providing a direct indicator of the cluster's age through comparison with theoretical isochrones. The position of the turnoff reflects the cluster's solar metallicity, which influences the evolutionary timescales and positions in color-magnitude diagrams. The in Messier 67 is well-populated, featuring evolved that have ascended after leaving the , with prominent K-type giants dominating the upper portions. These giants result from the expansion and cooling of post-turnoff as they ignite in shells around inert carbon-oxygen cores. Additionally, the cluster hosts a of , which represent a later phase where core burning occurs in a stable shell, following mass loss on the ; these provide insights into mass-loss efficiency and core masses around 0.5 solar masses. The sequence in Messier 67 forms a distinct cooling track in the color-magnitude diagram, comprising progenitors that evolved from stars above the turnoff mass, with cooling ages aligning closely with the cluster's total age of approximately 4.3 billion years. This sequence, extending from luminosities near MV=10M_V = 10 to fainter limits, has been instrumental in calibrating white dwarf cooling models due to the cluster's well-constrained distance and membership, revealing a mean white dwarf mass of about 0.6 solar masses consistent with solar-metallicity progenitors. Approximately 20–30 blue stragglers populate Messier 67, appearing brighter and bluer than the main-sequence turnoff, and are interpreted as products of binary mass transfer or stellar mergers that rejuvenate their evolution. These objects challenge standard single-star evolution by occupying regions above the turnoff, with masses estimated 1.2–1.5 times the turnoff value, and recent studies highlight uncertainties in evolutionary grids for their post-merger tracks, particularly in overshooting and rotation effects. Recent asteroseismology of s and in Messier 67, leveraging Kepler observations, has revealed acoustic modes that trace the deepening of convective envelopes as stars evolve from to phases. These p-modes show frequency shifts indicating rapid expansion of the convective zone, from depths comparable to the Sun in to encompassing nearly the entire star in , offering empirical constraints on mixing and structural changes during this transition.

Cluster Dynamics

Messier 67 exhibits clear signs of mass segregation, a dynamical process where more massive stars sink toward the cluster center while lower-mass stars are preferentially distributed in the outskirts. This segregation is evident in the central concentration of blue stragglers and binaries compared to single main-sequence stars, with the former showing a smaller half-mass radius of approximately 1.1 pc versus 3.8 pc for the overall . The process is quantified by the cluster's internal velocity dispersion of about 0.59 km/s, which facilitates energy equipartition among stars of varying masses. The half-mass relaxation time for Messier 67 is approximately 100 Myr, over which two-body encounters drive the observed mass segregation and overall dynamical . Given the cluster's age of around 4 Gyr, it has undergone roughly 40 relaxation times, rendering it a highly relaxed system where gravitational interactions have profoundly shaped its structure. Messier 67 follows an eccentric orbit within the , with a perigalacticon of about 6.8 kpc and an apogalacticon of 9.1 kpc, keeping it on a relatively stable path that largely avoids severe tidal disruptions from the Galactic disk or bulge. This orbital configuration contributes to the cluster's longevity despite its advanced age. Due to tidal forces from the , Messier 67 is experiencing ongoing , losing approximately 1% of its member stars per Gyr through dynamical ejection. At its current mass of roughly 2,000 M⊙ and with about 1,000 members, the cluster is expected to remain bound for another approximately 5 billion years. Stellar binaries play a supportive role in maintaining stability by injecting energy during close encounters, counteracting some relaxation-driven losses.

Exoplanets

Known Exoplanets

A survey of Messier 67 has identified four confirmed exoplanets and one candidate orbiting member stars: YBP1194, YBP401, YBP1514, S1429, and S978. These detections, primarily achieved through high-precision , reveal a population of close-in giant planets, with no transiting exoplanets confirmed to date. The survey utilized instruments such as HARPS at the ESO 3.6 m and SOPHIE at the Observatoire de Haute-Provence, supplemented by additional facilities like HARPS-N and HRS for follow-up observations. The planets around YBP1194 and YBP1514 were the first confirmed in the cluster, announced in 2014 after a six-year monitoring campaign of 88 probable members. YBP1194 b is a sub-Neptune-mass world with a minimum mass (m sin i) of 0.34 MJ and an orbital period of 6.9 days, while YBP1514 b has a minimum mass (m sin i) of 0.40 MJ and a period of 5.1 days; both orbit solar-like G-type dwarfs and exhibit moderate eccentricities (0.24 and 0.39, respectively). In 2016, a hot Jupiter was confirmed around the main-sequence star YBP401, with a minimum mass (m sin i) of approximately 0.42 MJ and a short period of 4.1 days, contributing to evidence of an elevated occurrence rate for such planets in dense clusters like M67. A giant planet candidate around the red giant S978, with an orbital period of about 510 days, was identified in 2017 through radial velocity monitoring but remains unconfirmed pending a full orbital solution. Most recently, in 2024, a warm Jupiter was confirmed orbiting the turn-off star S1429 using combined radial velocity and direct imaging constraints, yielding a minimum mass (m sin i) of 1.80 ± 0.20 MJ, period of 77.5 days, and semi-major axis of 0.38 AU. A planet candidate around Sand 364, initially reported in 2014 with a minimum of 1.54 MJ and period of 122 days, was later disproved in 2023 as a false positive attributable to stellar activity rather than an orbiting companion. This case underscores the challenges of distinguishing planetary signals from intrinsic stellar variability in evolved stars. The confirmed ' close orbits highlight potential dynamical stability issues in the cluster's dense environment, influenced by its ~4 Gyr age.
Host StarPlanetMinimum Mass (MJ)Orbital Period (days)Detection MethodDiscovery YearReference
YBP1194b0.346.92014Brucalassi et al. (2014)
YBP1514b0.405.12014Brucalassi et al. (2014)
YBP401b0.42 ± 0.054.12016Brucalassi et al. (2016)
S978bJovian-mass (exact value pending full orbital solution)~5102017 (candidate)Brucalassi et al. (2017)
S1429b1.80 ± 0.2077.5 + 2024Pasquini et al. (2024)

Planet Formation Insights

The exoplanets detected in Messier 67 offer key insights into formation and migration within the dense, dynamically interactive settings of open clusters. Observations from a study using ESO facilities, including HARPS and spectrographs, identified an elevated frequency of hot Jupiters around cluster members, estimated at about 5% compared to roughly 1% among similar field stars. This excess suggests that the cluster's high stellar density may enhance inward migration mechanisms, such as planet-disk interactions or events, facilitating the delivery of massive to short-period orbits more efficiently than in isolated systems. The endurance of these planetary systems over the cluster's age of approximately 4 billion years provides a critical test for prevailing planet formation paradigms, particularly the viability of long-term orbital stability in crowded environments. Messier 67's age, determined through isochrone fitting and white dwarf cooling sequences, aligns closely with the Sun's, making it an ideal analog for studying mature planetary architectures. The survival of , including examples like the Neptune-mass world orbiting a solar twin, implies that formation via core accretion—requiring extended timescales for solid core buildup followed by gas capture—can produce resilient systems capable of withstanding gravitational perturbations from nearby stars over gigayears, whereas disk instability models, which favor rapid assembly in massive protoplanetary disks, must account for equivalent dynamical resilience to explain such . Messier 67's solar ([Fe/H] ≈ 0), confirmed through high-resolution of member , further informs the metallicity-planet occurrence correlation by demonstrating diverse architectures around hosts without metal enrichment. While field star surveys indicate a strong bias toward around supersolar-metallicity hosts, potentially due to enhanced solid material availability for core growth, the cluster's findings reveal efficient formation at solar abundances, suggesting that environmental factors in clusters may compensate for lower metallicity and challenge assumptions of a strict threshold for giant planet production. A analysis of TESS data underscores potential threats to close-in exoplanets in aging clusters like Messier 67, where main-sequence turnoff stars are initiating envelope expansion akin to the Sun's future . The study finds evidence that post-main-sequence hosts frequently engulf nearby giants through tidal drag and stellar bloating, with destruction rates higher than previously modeled, implying that some of M67's short-period around subgiants may face imminent and implications for the cluster's evolving planetary demographics.

References

  1. https://science.nasa.gov/mission/hubble/science/explore-the-night-sky/hubble-messier-catalog/messier-67/
  2. https://apod.nasa.gov/apod/ap070809.html
  3. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Messier+67
  4. https://www.eso.org/public/news/eso1402/
  5. https://www.earth.com/news/warm-jupiter-spotted-in-a-four-billion-year-old-star-cluster/
  6. http://www.messier.seds.org/Mdes/dm067.html
  7. https://platestacks.cfa.harvard.edu/
  8. https://adsabs.harvard.edu/full/1917ApJ....45..164S
  9. https://adsabs.harvard.edu/full/1919ApJ....49..311S
  10. https://adsabs.harvard.edu/full/1930HarMo...2.....S
  11. https://arxiv.org/abs/2409.04581
  12. https://iopscience.iop.org/article/10.1088/0004-6256/142/2/59
  13. https://www.aanda.org/articles/aa/full_html/2023/06/aa43919-22/aa43919-22.html
  14. https://freestarcharts.com/messier-67
  15. https://www.aanda.org/articles/aa/pdf/2023/04/aa44723-22.pdf
  16. https://www.aanda.org/articles/aa/full_html/2019/07/aa35599-19/aa35599-19.html
  17. https://arxiv.org/pdf/astro-ph/0507239
  18. https://iopscience.iop.org/article/10.1088/0004-6256/150/3/97/pdf
  19. https://arxiv.org/abs/2407.03526
  20. https://iopscience.iop.org/article/10.3847/1538-3881/abe1ad
  21. https://arxiv.org/abs/astro-ph/9806172
  22. https://arxiv.org/abs/1310.6297
  23. https://arxiv.org/pdf/1803.04461
  24. https://academic.oup.com/mnras/article/532/2/2860/7708363
  25. http://www.messier.seds.org/m/m067.html
  26. https://iopscience.iop.org/article/10.3847/1538-4357/aad90b
  27. https://ui.adsabs.harvard.edu/abs/1998ApJ...504L..91R/abstract
  28. https://arxiv.org/abs/2502.18714
  29. https://arxiv.org/abs/1507.01949
  30. https://arxiv.org/abs/astro-ph/0507239
  31. https://arxiv.org/abs/1401.4905
  32. https://www.aanda.org/articles/aa/full_html/2016/08/aa27561-15/aa27561-15.html
  33. https://www.aanda.org/articles/aa/full_html/2017/07/aa27562-15/aa27562-15.html
  34. https://www.aanda.org/articles/aa/full_html/2024/06/aa49233-24/aa49233-24.html
  35. https://exoplanetarchive.ipac.caltech.edu/overview/NGC_2682_Sand_364
  36. https://www.ucl.ac.uk/news/2025/nov/ageing-stars-may-be-destroying-their-closest-planets
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