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Kepler-452b
Artist's impression of Kepler-452b (center), depicted here as a rocky planet in the habitable zone with extensive cloud cover. The actual appearance and composition of the exoplanet is unknown.
Discovery
Discovered byKepler Science team
Discovery siteKepler
Discovery date23 July 2015 (announced)
Transit
Designations
KOI-7016.01
Orbital characteristics
1.046+0.019
−0.015[1] AU
384.843+0.007
−0.012[1] d
Inclination89.806+0.134
−0.049
StarKepler-452
Physical characteristics
1.5+0.32
−0.22[1] R🜨
Mass5 ± 2[2] M🜨
1.9+1.5
−1.0 (est.) g[3]
TemperatureTeq: 265K+15
−13 (265 K (−8 °C; 17 °F))[1]

Kepler-452b (sometimes quoted to be an Earth 2.0 or Earth's Cousin[4][5] based on its characteristics; also known by its Kepler object of interest designation KOI-7016.01) is a candidate[6][7] super-Earth exoplanet orbiting within the inner edge of the habitable zone of the sun-like star Kepler-452 and is the only planet in the system discovered by the Kepler space telescope. It is located about 1,800 light-years (550 pc)[8] from Earth in the constellation of Cygnus.

Kepler-452b orbits its star at a distance of 1.04 AU (156 million km; 97 million mi) from its host star (nearly the same distance as Earth from the Sun), with an orbital period of roughly 385 days, has a mass at least three times that of Earth, and has a radius of around 1.6 times that of Earth, or around 60% larger than earth in size. It is the first potentially rocky super-Earth[9] planet discovered orbiting within the habitable zone of a very Sun-like star.[10] However, it is unknown if it is entirely habitable, as it is receiving slightly more energy from its star than Earth and could be subjected to a runaway greenhouse effect.

The Kepler space telescope identified the exoplanet, and its discovery was announced by NASA on 23 July 2015.[11] The planet is about 1,800 light-years (550 pc) away from the Solar System. At the speed of the New Horizons spacecraft, at about 59,000 km/h (16,000 m/s; 37,000 mph), it would take approximately 30 million years to get there.[12]

Physical characteristics

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Mass, radius and temperature

[edit]
Size comparison between Earth (left) and Kepler-452b (right) along with the similarities of their parent stars.

Kepler-452b has a probable mass five times that of Earth, and its surface gravity is nearly twice as much as Earth's, though calculations of mass for exoplanets are only rough estimates.[3] If it is a terrestrial planet, it is most likely a super-Earth with many active volcanoes due to its higher mass and density. The clouds on the planet would be thick and misty, covering much of the surface as viewed from space.

The planet takes 385 Earth days to orbit its star.[13] Its radius is 50% larger than Earth's, and lies within the conservative habitable zone of its parent star.[3][14] It has an equilibrium temperature of 265 K (−8 °C; 17 °F), a little warmer than Earth.

Host star

[edit]
Main article: Kepler-452

The host star, Kepler-452, is a G-type and has about the same mass as the sun, only 3.7% more massive and 11% larger. It has a surface temperature of 5757 K, nearly the same as the Sun, which has a surface temperature of 5778 K.[15] The star's age is estimated to be about 6 billion years old, about 1.5 billion years older than the Sun, which is estimated to have existed for 4.6 billion years. Kepler-452b has been in Kepler-452's habitable zone for most of its existence, a duration just over six billion years.[16]

From the surface of Kepler-452b, its star would look almost identical to the Sun as viewed from the Earth.[17] The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.426; therefore, it is too dim to be seen with the naked eye.

Orbit

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Kepler-452b orbits its host star with an orbital period of 385 days and an orbital radius of about 1.04 AU, nearly the same as Earth's (1 AU). Kepler-452b is most likely not tidally locked and has a circular orbit. Its host star, Kepler-452, is about 20% more luminous than the Sun (L = 1.2 L☉).

Potential habitability

[edit]
Comparison of Kepler-452b and related exoplanets with Earth.

It is not known if Kepler-452b is a rocky planet[4] with it being disputed whether its radius is small enough to indicate rocky planet[11] or too large to have not accumulated a voluminous gaseous envelope and be more Neptune-like.[18]

It is not clear if Kepler-452b offers a habitable environment. It orbits a G2V-type star, like the Sun, which is 20% more luminous, with nearly the same temperature and mass.[13] However, the star is roughly 6 billion years old, making it 1.5 billion years older than the Sun. At this point in its star's evolution, Kepler-452b is currently receiving 10% more energy from its parent star than Earth is currently receiving from the Sun.[10] If Kepler-452b is a rocky planet, it may be subject to a runaway greenhouse effect similar to that seen on Venus.[19]

"Delayed" runaway greenhouse effect

[edit]

However, due to the planet Kepler-452b being 50 percent bigger in terms of size, it is likely to have an estimated mass of 5 M🜨, which could allow it to hold on to any oceans it may have for a longer period, preventing Kepler-452b from succumbing to runaway greenhouse effect for another 500 million years.[19] This, in turn, would be accompanied by the carbonate–silicate cycle being "buffered", extending its lifetime due to increased volcanic activity on Kepler-452b.[20] This could allow any potential life on the surface to inhabit the planet for another 500–900 million years before the habitable zone is pushed beyond Kepler-452b's orbit.

Discovery and follow-up studies

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In 2009, NASA's Kepler space telescope was observing stars on its photometer, the instrument it uses to detect transit events, in which a planet crosses in front of and dims its host star for a brief and roughly regular time. In this last test, Kepler observed 50000 stars in the Kepler Input Catalog, including Kepler-452; the preliminary light curves were sent to the Kepler science team for analysis, who chose obvious planetary companions from the bunch for follow-up by other telescopes. Observations for the potential exoplanet candidates took place between 13 May 2009 and 17 March 2012. Kepler-452b exhibited a transit that occurred roughly every 385 days, and it was eventually concluded that a planetary body was responsible. The discovery was announced by NASA on 23 July 2015.[11]

At a distance of nearly 1,800 light-years (550 pc), Kepler-452b is too remote for current telescopes or the next generation of planned telescopes to determine its true mass or whether it has an atmosphere. The Kepler space telescope focused on a single small region of the sky but next-generation planet-hunting space telescopes, such as TESS and CHEOPS, will examine nearby stars throughout the sky with follow up studies planned for these closer exoplanets by the James Webb Space Telescope and future large ground-based telescopes to analyze their atmospheres, determine masses, and infer compositions.

A study in 2018 by Mullally et al. claimed that statistically, Kepler-452b has not been proven to exist and must still be considered a candidate.[6] However, Kepler-452b is still a possible planet and has not been shown to be a false positive.[6]

SETI targeting

[edit]

Scientists with the SETI (Search for Extraterrestrial Intelligence Institute) have already begun targeting Kepler-452b, the first near-Earth-size world found in the habitable zone of a Sun-like star.[21] SETI Institute researchers are using the Allen Telescope Array, a collection of 6-meter (20 feet) telescopes in the Cascade Mountains of California, to scan for radio transmissions from Kepler-452b. As of July 2015, the array has scanned the exoplanet on over 2 billion frequency bands, with no result. The telescopes will continue to scan over a total of 9 billion channels, searching for alien radio analysis.[21]

Observation and exploration

[edit]

Kepler-452b is 1,800 light-years (550 parsecs) from Earth. The fastest current spacecraft, the New Horizons uncrewed probe that passed Pluto in July 2015, travels at just 56,628 km/h (15,730 m/s; 35,187 mph; 0.00037853 AU/h).[5] At that speed, it would take a spacecraft about 26 million years to reach Kepler-452b from Earth, if it were going in that direction.[5]

Notable Exoplanets – Kepler Space Telescope
Comparison of small planets found by Kepler in the habitable zone of their host stars.
[edit]
  • A diagram of the orbit of Kepler-452b within the Kepler-452 system, as compared to the inner Solar System and Kepler-186 system, and their respective projected habitable zones.
    A diagram of the orbit of Kepler-452b within the Kepler-452 system, as compared to the inner Solar System and Kepler-186 system, and their respective projected habitable zones.

See also

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References

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

Kepler-452b

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from Grokipedia
Kepler-452b is a super-Earth exoplanet orbiting the Sun-like star Kepler-452, located about 1,800 light-years away in the constellation Cygnus. Discovered in 2015 by NASA's Kepler space telescope using the transit method, it has a radius of 1.63 ± 0.22 times that of Earth and completes one orbit every 384.8 days at a semi-major axis of 1.046 AU, positioning it within the habitable zone of its host star where liquid water might exist under suitable conditions. The host star is a G2-type star with an of 5432 ± 45 , a radius 1.16 ± 0.02 times that of the Sun, a 1.02 ± 0.13 times solar, and an age of approximately 6 billion years—1.5 billion years older than the Sun. This star is approximately 16% larger and 5% brighter than the Sun, delivering an insolation flux to Kepler-452b that is 1.10 times Earth's, resulting in an equilibrium temperature of 265 ± 14 assuming a of 0.3. Although the planet's mass remains undetermined due to the absence of data, statistical models indicate a probable rocky composition with a mass estimated at approximately 3.3 masses, making it a potential candidate for studies. Dubbed 's "older cousin" by , Kepler-452b represents a milestone as the first near--sized world found in the of a G-type star similar to the Sun, advancing the search for potentially life-bearing exoplanets.

Discovery and confirmation

Kepler mission detection

Kepler-452b was detected during the analysis of photometric data collected by NASA's during its primary mission, which operated from 2009 to 2013. The signal was identified using the Kepler Science Operations Center (SOC) pipeline version 9.2 in May 2014, with confirmation following reprocessing of the full four-year dataset (quarters Q1–Q17) in November 2014. The detection relied on the transit method, which identifies exoplanets by measuring periodic dips in a star's brightness caused by a passing in front of it from the observer's perspective. For Kepler-452b, four transits were observed, one each in quarters Q3, Q7, Q11, and Q15, spaced approximately every 385 days due to the 's . Each transit lasted about 10.5 hours and produced a brightness decrease of roughly 200 parts per million (0.02%), allowing initial estimates of the planet's radius relative to its host star, , a Sun-like G2-type star. The transit signal was statistically significant at 9.7σ, with a probability of 2.32 × 10^{-16}, indicating a highly unlikely chance of it being noise. Kepler-452b initially appeared as a in the Kepler catalog of potential transiting , subjected to further to rule out false positives such as eclipsing binaries or instrumental artifacts. Validation involved assessing the false positive probability (FPP) using tools like the analysis, which yielded odds of 424:1 in favor of a true planetary transit over alternative scenarios. Key parameters derived from the detection include an of 384.843^{+0.007}_{-0.012} days and a semi-major axis of approximately 1.046 AU, placing the in a nearly similar in scale to Earth's around the Sun. These values were obtained through modeling the transit timing and depth in the Kepler .

Announcement and validation studies

announced the discovery of Kepler-452b on July 23, 2015, through a describing it as "Earth's bigger, older cousin," highlighting its Earth-like size and position in the of a Sun-like star. In the same press release, NASA stated that “This exciting result brings us one step closer to finding an Earth 2.0.” The announcement was based on transit data from the full Kepler primary mission dataset (quarters Q1–Q17). Subsequent validation efforts faced challenges due to higher false positive rates for long-period, small-radius candidates. A 2018 study by Mullally et al. analyzed instrumental artifacts in Kepler data, concluding that statistical validation alone could not confirm Kepler-452b at the 99% level, estimating its true transit probability at around 16% under conservative assumptions and questioning the reliability of similar long-period detections. A 2019 study by Burke et al. re-evaluated small, long-period Kepler candidates using updated false positive models, occurrence rates, and Bayesian techniques, finding that Kepler-452b no longer achieves 99% in the planetary , with a probability relative to the of 0.86, and thus not statistically validated, in agreement with Mullally et al. (2018). Despite these concerns, the was retained as a likely , though with reduced compared to shorter-period planets. In October 2025, Ramirez et al. reassessed Kepler Earth-like candidates using data-driven null signal templates to estimate probabilities (FAP), accounting for and noise. The study found Kepler-452b has an FAP below 1%, supporting its statistical validity as a strong planetary candidate without requiring independent or imaging detection. Data Release 3, released in 2022 with subsequent analyses in 2023, refined the distance to the Kepler-452 to approximately 1,800 light-years (550 parsecs), improving upon earlier estimates through precise measurements. of the full Kepler transit dataset revealed no signals indicative of additional in the system.

Host system

Kepler-452 star properties

Kepler-452 is a G-type main-sequence star located in the constellation Cygnus, approximately 1,800 light-years from Earth. Its coordinates are right ascension 19h 44m 00.883s and declination +44° 16′ 39.″22 (J2000 epoch), placing it in the field of view observed by the Kepler Space Telescope. With an apparent magnitude of 13.7 in the visual band, the star is too faint to be seen with the naked eye and requires a telescope for observation. The star has a spectral classification of , making it a Sun-like star with an of 5,757 ± 85 K, slightly cooler than the Sun's 5,772 K. Its measures 1.11^{+0.15}{-0.09} times that of the Sun, and its mass is 1.037^{+0.054}{-0.047} solar masses, indicating a modestly larger and more massive body than the Sun. The is approximately 1.2 times solar, derived from the Stefan-Boltzmann relation using the measured and . exhibits a of [Fe/H] = +0.21 ± 0.09 dex, indicating it is slightly more metal-rich than the Sun, which may influence formation processes around it. Estimated to be about 6 ± 2 billion years old, is roughly 1.5 billion years older than the Sun, placing it in a mature phase of its main-sequence evolution. This advanced age suggests the star has maintained a stable over billions of years, with its gradually expanding outward at a rate of about 1.5 cm per year due to the star's increasing brightness. Such stability provides a long-term environment conducive to potential , contrasting with younger, more variable G-type stars.

Orbital characteristics

Kepler-452b completes one orbit around its host star, Kepler-452, every 384.843 days, with an uncertainty of +0.007/−0.012 days. This orbital period places the planet in the habitable zone of the G2-type star. The semi-major axis of the orbit measures 1.046 AU (+0.019/−0.015 AU), approximately 5% farther from the star than Earth's distance from the Sun. The orbit is consistent with a circular path, with an eccentricity of 0 as derived from transit data analysis. Transit observations indicate an orbital inclination of 89.806° (+0.134/−0.049°), nearly edge-on relative to our line of sight. No additional planetary companions have been detected in the Kepler-452 system, supporting the stability of this isolated orbit. The planet receives an insolation flux of 1.10 (+0.29/−0.22) times that of Earth, calculated using the formula F=L⋆4πa2F = \frac{L_\star}{4\pi a^2}, where L⋆L_\star is the stellar luminosity (approximately 1.2 times solar) and aa is the semi-major axis. Given the large orbital separation, tidal locking is not expected within the system's age of about 6 billion years, as the synchronization timescale exceeds 10 Gyr for Earth-like parameters.

Physical properties

Size, mass, and density

Kepler-452b has an estimated of 1.63±0.231.63 \pm 0.23 radii (R\EarthR_\Earth), determined from the depth of its transit relative to the host star's . The transit depth ΔF/F=(Rp/R⋆)2\Delta F/F = (R_p/R_\star)^2 provides the planetary once the stellar is established through and . This measurement depends on the accuracy of the host star's parameters, with the stellar estimated at 1.11−0.09+0.151.11^{+0.15}_{-0.09} solar radii. Direct mass measurements are unavailable due to the lack of detection, as the host star is too faint and distant (approximately 1,800 light-years away) for precise with current instruments. Mass estimates from empirical mass-radius relations for s suggest a value around 5 M\EarthM_\Earth. A 2023 study estimates the mass at 3.78 ± 2.29 Earth masses using Bayesian retrieval methods. If around 5 Earth masses, Kepler-452b would classify as a massive , but the absence of direct measurement introduces significant uncertainty. Assuming a rocky composition, the implied density is approximately 4–5 g/cm³, consistent with a structure featuring a silicate mantle, iron core, and possible water layer. Probabilistic models indicate a 49%–62% likelihood of a rocky makeup, with alternatives including a volatile-rich envelope that could lower the density. A 2018 study raised concerns about potential false positives, such as blended eclipsing binaries, which could dilute the transit depth and inflate size estimates, but subsequent analyses, including a 2025 study, confirm its validity with a false alarm probability below 1%.

Temperature and surface conditions

The equilibrium temperature of Kepler-452b, which represents the effective temperature assuming no internal heat sources or atmospheric effects, is estimated at 265 ± 15 K (-8 ± 15 °C) under the assumptions of a Bond albedo of 0.3 and full redistribution of absorbed stellar heat across the planet's surface. This value is derived from the planet's insolation flux of 1.10 ± 0.29 times that of Earth, calculated using the formula for effective insolation Seff/S⊕=a−2(Teff/T⊙)4(R∗/R⊙)2S_{\rm eff}/S_\oplus = a^{-2} (T_{\rm eff}/T_\odot)^4 (R_*/R_\odot)^2, where aa is the semi-major axis in AU, TeffT_{\rm eff} is the stellar effective temperature, and R∗R_* and R⊙R_\odot are the stellar and solar radii, respectively. The equilibrium temperature is then obtained via the blackbody relation Teq=[F(1−A)4σ]1/4T_{\rm eq} = \left[ \frac{F (1 - A)}{4 \sigma} \right]^{1/4}, with FF as the incident flux, AA the Bond albedo, and σ\sigma the Stefan-Boltzmann constant. Without an atmosphere, this temperature suggests a cold, frozen surface similar to a perpetual winter on , but the presence of a substantial atmosphere could significantly alter conditions through a . Models indicate that an Earth-like atmosphere with comparable CO₂ levels would raise the surface to around 300 (27 °C) in tropical regions, potentially allowing liquid under clear-sky conditions and moderate atmospheric pressures. For a zero-albedo scenario with no atmosphere or greenhouse forcing, the equilibrium drops to approximately 265 , emphasizing the planet's baseline thermal state driven primarily by stellar irradiation. Assuming a rocky composition with a mass of about 5 masses—consistent with models for its 1.6 -radius size—the surface on Kepler-452b is estimated at roughly 1.9 times 's (approximately 18.6 m/s²). This elevated arises from the relation g=GMR2g = \frac{GM}{R^2}, where higher outweighs the increase in radius squared, leading to stronger retention of any primordial atmosphere and potential for a thicker crust compared to . The greater also implies enhanced radiogenic heating from in the core and mantle, which could drive geological activity such as , though is negligible due to the planet's wide orbit. Given its of 385 days at 1.05 AU from the host star, Kepler-452b is unlikely to be tidally synchronized, allowing for a period similar to Earth's, potentially in the range of 20–30 hours based on expectations for non-locked terrestrial worlds. This would support a dynamic day-night cycle, influencing local patterns and heat distribution if an atmosphere is present.

Habitability assessment

Habitable zone placement

The (HZ) refers to the orbital region around a star where a could sustain water on its surface, provided it has suitable atmospheric conditions. For a G2V star like the Sun, the conservative HZ—bounded by the inner runaway greenhouse limit (where water vapor feedback leads to atmospheric loss) and the outer maximum greenhouse limit (where CO₂ condensation prevents further warming)—spans approximately 0.95 to 1.67 AU. This definition, derived from one-dimensional climate models, emphasizes boundaries where Earth-like habitability is most plausible without extreme atmospheric adjustments. Kepler-452, a G2V star with a 1.21 times that of the Sun, has a correspondingly shifted HZ, scaled outward by the square root of its luminosity ratio. Kepler-452b orbits at a semi-major axis of 1.05 AU, positioning it near the inner edge of this conservative HZ. The planet receives approximately 10% more incident stellar flux than (1.1 times the terrestrial value), which places it just beyond the strict conservative boundary but firmly within the broader optimistic HZ (extending to the "recent Venus" limit). This flux level suggests potential for liquid water if the planet maintains an Earth-analog atmosphere, though higher insolation could challenge long-term stability without mitigating factors like . The star's estimated age of 6 billion years implies evolutionary changes in the HZ due to gradual increases in during its main-sequence phase. Over time, this outward migration of the HZ has ensured that Kepler-452b has remained within bounds for at least the past 5 billion years, starting from a position analogous to an early Venus-like orbit relative to its then-fainter host star. The relative stability of G2V stars like extends this window, projecting another approximately 3 billion years before the inner HZ edge surpasses the planet's orbit. The (ESI), a metric quantifying planetary resemblance to based on radius, density, , and surface , yields a value of ~0.83 for Kepler-452b, reflecting its moderate Earth-likeness primarily driven by size and insolation.

Climate evolution models

Theoretical models of Kepler-452b's climate evolution emphasize the planet's potential for a delayed runaway greenhouse effect compared to Venus, owing to its estimated higher surface gravity—approximately 1.6 times Earth's—and the star's increased insolation of about 1.1 times Earth's flux, which collectively slow the rate of atmospheric water loss through hydrodynamic escape. These factors suggest that, if Kepler-452b formed with an Earth-like water inventory, liquid water could persist on its surface for an additional 500–900 million years before a full runaway greenhouse renders it uninhabitable, extending the post-formation habitability window beyond what simpler one-dimensional models predict. Three-dimensional general circulation models (GCMs), such as adaptations of the Community Climate System Model (CCSM3), have been employed to simulate Kepler-452b's atmospheric dynamics, incorporating coupled ocean-atmosphere interactions under varying CO₂ concentrations. These simulations indicate a moist threshold at roughly 1.1 times Earth's incident stellar , beyond which begins to accumulate in the , accelerating escape and leading to over geological timescales. The equilibrium temperature, influenced by this , plays a key role in modulating forcing in these models. Hypotheses regarding atmospheric composition posit a buildup of CO₂ and due to volcanic and limited silicate under higher , potentially stabilizing a thick atmosphere if initial abundances were substantial. Interior structure models suggest Kepler-452b could be water-rich, with a significant H₂O fraction (up to 50% or more), supporting the possibility of an with global liquid coverage rather than a surface dominated by continents. If microbial life were present, biosignatures such as stratospheric oxygen or tropospheric could theoretically accumulate in the atmosphere, detectable via high-resolution , though the planet's distance (approximately 1,800 light-years) and faintness pose significant observational challenges with current telescopes. Studies from 2015 to 2023, including Jenkins et al.'s analysis of tidal effects on orbital evolution and interior composition, highlight how tidal dissipation might influence long-term climate stability without leading to locking, while GCM-based works like those by Haqq-Misra et al. refine limits. No major updates have emerged since these foundational efforts, leaving gaps in modeling that could be addressed with James Webb Space Telescope-era constraints on atmospheric retrievals, though Kepler-452b remains a low-priority target due to its brightness constraints.

Follow-up observations

SETI searches

Following the discovery announcement of Kepler-452b on July 23, 2015, the launched a targeted radio search for technosignatures from the system using the (ATA) in , with observations commencing in late July 2015. The initial effort scanned frequencies from 1 to 9 GHz, focusing on the star's position in the constellation Cygnus to account for the planet's orbital location. The methodology involved searches for artificial signals, processing data across approximately 10^4 to 10^6 channels with resolutions of 0.7 to 100 Hz, and integration times extending up to several hours per observation to enhance sensitivity for weak or transient emissions. An anticoincidence filter was applied to reject terrestrial interference, while monitoring for relative accelerations between the transmitter and receiver ranging from -0.3 to 0.3 m/s² to detect potential Doppler shifts from orbiting sources. Observations conducted between 2015 and 2016, totaling part of the ATA's ~19,000 hours of monitoring, yielded no detections of artificial signals from the system, confirming the system's radio quietness at the surveyed frequencies. The searches assumed the presence of an advanced capable of isotropic or directed , but the planet's distance of about 1,800 light-years severely constrains detectable , requiring signals on the order of 180–310 × 10^{-26} W/m² for identification. As of 2025, no additional dedicated SETI campaigns targeting Kepler-452b have been reported, though expanded efforts by initiatives like offer potential for future high-sensitivity radio surveys of habitable-zone .

Future exploration prospects

The host star has an apparent visual magnitude of 13.7, rendering it too faint for ground-based of its without advanced , and current facilities lack the sensitivity for detailed atmospheric analysis of Kepler-452b at this distance. As of November 2025, the (JWST) has not conducted targeted observations of Kepler-452b, primarily due to the system's distance of approximately 1,800 light-years, which limits signal-to-noise ratios for transmission or emission even with JWST's capabilities. Key gaps persist in characterizing Kepler-452b, including the absence of a mass measurement, which relies on detecting the star's wobble—a challenge given the faintness and the planet's estimated mass of about 5 masses (from statistical models assuming composition). to probe potential atmospheres would require next-generation ground-based telescopes like the (ELT), expected to achieve first light in the late 2020s, or space-based platforms for sufficient contrast against the host star. Proposed future missions offer pathways for direct imaging and . The Habitable Worlds Observatory (HWO), slated for launch in the 2030s, could employ coronagraphy to image and spectrally analyze habitable-zone exoplanets around Sun-like stars, potentially including systems like if prioritized in target lists. Similarly, concepts from the (LUVOIR) mission emphasize atmospheric of super-Earths in habitable zones via high-contrast imaging, enabling detection of biosignatures such as oxygen or . Interstellar travel to Kepler-452b remains infeasible with current propulsion technologies. At the speed of (approximately 14 km/s), the journey would take over 38 million years, based on the updated distance of 1,800 light-years; relativistic probes or advanced concepts like laser-driven sails are speculative and unproven for crewed missions. In the 2025 outlook, missions like TESS continue to discover Earth-sized planets in habitable zones around Sun-like stars, while the mission (launch planned for 2026) will focus on similar systems for asteroseismology and transit follow-up, though Kepler-452b itself is not a primary target due to its distance and Kepler-era origins.

References

  1. https://science.nasa.gov/exoplanet-catalog/kepler-452-b/
  2. https://exoplanetarchive.ipac.caltech.edu/overview/Kepler-452%20b
  3. https://iopscience.iop.org/article/10.1088/0004-6256/150/2/56
  4. https://www.nasa.gov/news-release/nasas-kepler-mission-discovers-bigger-older-cousin-to-earth/
  5. https://www.nasa.gov/wp-content/uploads/2015/07/ms-r1b.pdf
  6. https://iopscience.iop.org/article/10.3847/1538-3881/aabae3
  7. https://iopscience.iop.org/article/10.3847/1538-3881/aafb79
  8. https://www.pnas.org/doi/10.1073/pnas.2513927122
  9. https://exoplanetarchive.ipac.caltech.edu/overview/Kepler-452b
  10. https://exoplanetarchive.ipac.caltech.edu/overview/Kepler-452
  11. https://arxiv.org/abs/0902.0952
  12. https://oro.open.ac.uk/102762/1/CLAY_SXP390_RVOR.pdf
  13. https://academic.oup.com/mnras/article/470/2/2270/3862545
  14. https://arxiv.org/abs/1507.06723
  15. https://iopscience.iop.org/article/10.3847/2041-8213/aa56c4
  16. https://www.space.com/30034-earth-cousin-exoplanet-kepler-452b-life.html
  17. https://doi.org/10.1088/0004-637X/765/2/131
  18. https://doi.org/10.1088/0004-6256/150/2/56
  19. https://www.space.com/30114-seti-alien-life-kepler-452b-earth-cousin.html
  20. https://www.nature.com/articles/nature.2015.18048
  21. https://arxiv.org/abs/1607.04207
  22. https://breakthroughinitiatives.org/initiative/1
  23. https://www.exoplanet.eu/catalog/kepler_452_b--2420/
  24. https://www.star-facts.com/kepler-452/
  25. https://asd.gsfc.nasa.gov/luvoir/
  26. https://arxiv.org/abs/1912.06219
  27. https://www.aanda.org/articles/aa/full_html/2022/09/aa41640-21/aa41640-21.html
  28. https://spectrum.ieee.org/how-space-telescopes-will-find-earth-20
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