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AR Scorpii
AR Scorpii
AR Scorpii
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AR Scorpii

Artist’s impression of AR Scorpii.
Observation data
Epoch J2000      Equinox J2000
Constellation Scorpius
Right ascension 16h 21m 47.28s[1]
Declination −22° 53′ 10.3″[1]
Characteristics
Apparent magnitude (G) 13.6 - 16.9[2]
White dwarf
Evolutionary stage White dwarf
Red dwarf
Evolutionary stage Main sequence
Spectral type M5[3]
Astrometry
Proper motion (μ) RA: 9.707[4] mas/yr
Dec.: −51.469[4] mas/yr
Parallax (π)8.4918±0.0408 mas[4]
Distance384 ± 2 ly
(117.8 ± 0.6 pc)
Details
White dwarf
Mass0.8[5] M☉
Radius0.01[5] R☉
Radius7000[5] km
Rotation1.95[3] minutes
Red dwarf
Mass0.28 - 0.45[3] M☉
Other designations
AR Sco, 2MASS J16214728-2253102
Database references
SIMBADdata

AR Scorpii (AR Sco) is a binary pulsar that consists of a white dwarf and a red dwarf.[3] It is located close to the ecliptic plane in the constellation Scorpius. Parallax measurements made by Gaia put the system at a distance of about 380 light-years (120 parsecs).[4]

In 1904 Henrietta Swan Leavitt and Edward Charles Pickering announced the discovery of this variable star.[6] It was given its variable star designation, AR Scorpii, in 1914.[7]

A broadband optical light curve for AR Scorpii, plotted from Kepler data[8]

AR Scorpii is the first "white dwarf-pulsar" to be discovered.[9] Its unusual nature was first noticed by amateur astronomers.[10] The 3.56-hour period in AR Scorpii's light curve caused it to be misclassified as a Delta Scuti variable, but in 2016, this period was found to be the binary orbital period. In addition, the system shows very strong optical, ultraviolet, and radio pulsations originating from the red dwarf with a period of just 1.97 minutes, which is a beat period from the orbital rotation and the white dwarf spin.[3] These pulsations occur when a relativistic beam from the white dwarf sweeps across the red dwarf, which then reprocesses the beam into the observed electromagnetic energy. Although the white dwarf shows evidence of accretion in the past, at present it is not accreting significantly, and the system is powered by the spin-down of the white dwarf.[9][5] The white dwarf's rotation will slow down on a timescale of 107 years.[5] It has a radius of about 7×103 km,[5] about the same size as Earth.

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References

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AR Scorpii

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AR Scorpii is a system in the constellation , approximately 380 light-years from Earth, consisting of a rapidly spinning and a cool M-type red dwarf star orbiting each other every 3.6 hours. The , roughly Earth-sized but 200,000 times denser, possesses a of approximately 15 million gauss (about 30 million times stronger than Earth's) and rotates with a period of 1.97 minutes, accelerating electrons to near-light speeds and producing intense beams of radiation and particles that periodically illuminate the companion star. This interaction causes dramatic variations observable from to radio wavelengths, making AR Scorpii the first known , a unique counterpart to pulsars but powered by different mechanisms without accretion. Discovered in 2015 by amateur astronomers and confirmed through observations with the European Southern Observatory's and other facilities, AR Scorpii was initially misclassified as a star since the 1970s due to its periodic fluctuations. Unlike traditional pulsars, its emissions arise from generated by the white dwarf's magnetic field interacting with the 's wind and atmosphere, rather than a rotating star's lighthouse effect, and the system shows no evidence of between the stars. The has about one-third the mass of the Sun, and the close separation of roughly 1.4 million kilometers amplifies the beaming effects, with pulses brightening the system up to 40% in polarization. Since its identification, AR Scorpii has revealed ongoing evolutionary changes, including rapid variations in pulse strength and asymmetry observed in light curves, suggesting dynamic interactions or orbital modulations over timescales of years; it remains the prototype for pulsars, with a second similar system discovered in 2023. These properties position it as key for studying magnetism and binary evolution, with emissions detected across the spectrum from X-rays to radio, providing insights into rare non-accreting polar systems.

Discovery and observation history

Early discovery

AR Scorpii was first identified as a in 1971 through photographic observations conducted by N. A. Satyvaldiev at the Astronomical Institute of the Academy of Sciences of the Turkmen SSR. These initial detections noted periodic brightness fluctuations, leading to its prompt classification as a δ Scuti variable, a type of pulsating star characterized by short-period radial oscillations. The designation AR Scorpii was assigned within the standard nomenclature for variable stars in , reflecting its position in the constellation and the sequential cataloging of such objects. Early light curves revealed an apparent visual magnitude varying between approximately 13.6 and 16.9, with the dominant 3.56-hour periodicity interpreted as evidence of intrinsic stellar pulsation rather than orbital motion. The star lies in the constellation , close to the plane, at equatorial coordinates RA 16ʰ 21ᵐ 47.³, Dec. −22° 53′ 12″ (J2000.0). Subsequent reobservations in 2016 unveiled its binary nature, overturning the long-standing single-star interpretation.

Characterization as a white dwarf binary

In May 2015, a group of amateur astronomers noticed unusual and erratic variability in AR Scorpii and contacted professional astronomers, prompting intensive observations. In 2016, AR Scorpii was identified as a binary system consisting of a white dwarf and a low-mass cool companion through optical photometry and spectroscopy, which revealed that the 3.56-hour photometric variability arises from the binary orbital period rather than intrinsic stellar pulsations. This breakthrough, led by Marsh et al., utilized data from the South African Large Telescope (SALT) to resolve the system's components and emission properties, marking a departure from its earlier 20th-century misclassification as a Delta Scuti variable star. The observations demonstrated coherent pulsations every 1.97 minutes spanning ultraviolet, optical, and radio wavelengths, establishing AR Scorpii as the first known white dwarf pulsar powered by the spin-down of its rapidly rotating white dwarf primary. Follow-up studies in 2016–2017, including polarimetric observations by Buckley et al., provided further evidence of the system's pulsar-like nature through the detection of strongly linearly polarized pulses reaching up to 40% polarization, indicative of beamed synchrotron emission from relativistic electrons interacting with the white dwarf's magnetosphere. These polarimetric data, collected using instruments at (ESO) facilities such as the (VLT), confirmed the emission's directional beaming and its modulation with the white dwarf's spin and orbital beat periods. Multi-wavelength confirmations extended to radio arrays, including early detections with the Australia Telescope Compact Array (ATCA), which corroborated the pulsed emission across the spectrum. The distance to AR Scorpii was precisely measured at 384 ± 2 light-years (117.8 ± 0.6 parsecs) via parallax from Gaia Data Release 2, providing essential context for its luminosity and energy output. These post-2016 observations collectively redefined AR Scorpii as a unique spin-powered binary pulsar, distinct from typical cataclysmic variables.

System parameters

Components

The AR Scorpii binary system consists of a white dwarf primary and a low-mass red dwarf secondary, orbiting each other in a close configuration. The primary is a hydrogen-atmosphere (DA-type) with an estimated mass of approximately 0.8 M⊙, a radius of about 7,000 km—comparable to that of —and a of log g ≈ 8. Its has an upper limit of < 9,750 . The secondary is an M5-type with a mass in the range 0.28–0.45 M⊙ (roughly one-third of the ), a radius of approximately 0.3 R⊙, and an of about 3,200 ; its illuminated hemisphere contributes to the system's reprocessed emission. The system is viewed nearly edge-on, with an inclination close to 90°, which enables deep eclipses and pronounced photometric variations. No exoplanets or debris disks are known in the AR Scorpii system.

Orbit and rotation

AR Scorpii is a close consisting of a primary and a low-mass M-dwarf secondary in a nearly with a period of 3.56 hours. The has low eccentricity, consistent with a circular configuration, and a semi-major axis of approximately 1.2 R⊙ for the relative , driven primarily by the dynamics of the with a mass of about 0.8 M⊙. The semi-amplitude of the secondary is K ≈ 295 km s⁻¹, reflecting the tight orbital motion. The rotates with a spin period of 1.95 minutes (117 s), which is the shortest known rotation period among white dwarfs. This rapid spin interacts with the orbital motion to produce beat frequencies, resulting in observed pulsations at a period of 1.97 minutes. The M-dwarf secondary fills its but exhibits negligible to the , classifying AR Scorpii as a non-accreting system. Gaia astrometry provides the systemic proper motion of μα cos δ = 9.69 ± 0.05 mas yr⁻¹ and μδ = −51.49 ± 0.04 mas yr⁻¹, with a low systemic radial velocity component indicating Galactic space velocities of (U, V, W) ≈ (15, −5, −15) km s⁻¹.

Variability and pulsations

Light curve features

The optical light curve of AR Scorpii exhibits a double-peaked orbital modulation with a period of 3.56 hours, characterized by high and low states arising from the beamed illumination of the red dwarf's hemisphere facing the white dwarf. This modulation shows flux variations by a factor of up to 20 in the g' band, with the system transitioning between brighter high states and dimmer low states over the orbital cycle. Superimposed on this orbital variation are rapid beat pulsations at a period of 1.97 minutes, resulting from the interaction between the white dwarf's spin and the orbital motion. These pulsations feature primary and secondary pulses, with the flux increasing by a factor of four within 30 seconds at pulse peaks; the primary pulse was approximately twice as strong as the secondary in 2015 observations, but by 2023, their amplitudes had equalized. The beat pulse amplitudes also vary over the orbital phase, with stronger pulsations during the high orbital state due to enhanced illumination. The optical emission is highly polarized, with reaching up to 40% at peaks and varying in synchronization with the 1.97-minute beat cycle. The polarization angle swings by approximately 360° over one spin phase, reflecting the . Over a nine-year baseline from 2015 to 2023, the relative amplitudes of the beat pairs have shown secular , consistent with a long-term cycle of at least 40 years driven by . This indicates that amplitudes are expected to maximize in the coming decade before returning to greater asymmetry.

Multi-wavelength observations

Ultraviolet observations of AR Scorpii have revealed pulsations with the characteristic 1.97-minute spin period of the , alongside orbital modulation on the 3.56-hour timescale, mirroring the behavior seen in optical light curves. Archival data from the first detected these UV pulses, confirming non-thermal emission extending from optical wavelengths into the regime. Follow-up observations with the Swift Ultraviolet/Optical Telescope (UVOT) further characterized the UV variability, showing pulsed flux with amplitudes up to 50% and spectral hardening during high states, consistent with processes involving relativistic electrons. In the radio domain, AR Scorpii exhibits pulsed emission across 0.2–10 GHz, marking it as the first binary detected at radio frequencies. Observations with the Karl G. Jansky Very Large Array () resolved coherent pulses at the white dwarf's spin period and its beat frequency with the , with flux densities reaching several millijansky and high indicative of from relativistic electrons in the system's . Complementary MeerKAT observations in the 0.6–1.4 GHz range confirmed these pulses, revealing orbital phase-dependent variability and establishing the emission's origin in magnetically confined particle acceleration near the white dwarf. The shows a flat to inverted shape, with peak fluxes modulated by up to 100% on spin timescales. Submillimeter observations conducted in 2022 using the Submillimeter Array at 220 GHz and 345 GHz detected flux densities of 124 ± 2 mJy and 86 ± 11 mJy, respectively, with pulsations at twice the spin frequency (58.26 s period) at 6% amplitude in the 220 GHz band—the first direct detection of the spin period in this regime. The indicates a break in emission around 200 GHz. X-ray observations conducted between 2016 and 2020 using and detected soft emission below 2 keV, dominated by thermal plasma from the heated atmosphere of the M-dwarf companion, with an unabsorbed luminosity of approximately 102910^{29} erg s−1^{-1}. The displays strong orbital modulation, peaking when the M dwarf's irradiated face is visible, but lacks detectable pulsations at the 's spin period, suggesting the emission arises from shocked regions rather than direct beaming. Spectral fits indicate multi-temperature plasma (0.1–0.6 keV) with low , consistent with coronal activity enhanced by the 's magnetic influence. Infrared photometry from surveys such as and WISE reveals excess emission attributable to from the irradiated face of the , where the white dwarf's beamed radiation heats the companion's surface to temperatures exceeding 4000 K. This component dominates the near- to mid-infrared spectrum, showing orbital variability aligned with the optical and contributing to the overall as a blackbody-like tail. No gamma-ray emission has been detected from AR Scorpii, with Fermi Large Area Telescope observations over a decade providing upper limits on the integral flux above 100 MeV at 2×10−122 \times 10^{-12} erg cm−2^{-2} s−1^{-1}, constraining potential high-energy extensions of the .

Physical model

Emission mechanism

The emission in AR Scorpii arises from a non-accreting polar-like model, where the rapidly rotating , with a spin period of approximately 117 seconds, powers the system through loss. The 's , estimated at ~15 megagauss (MG) based on 2025 submillimeter observations, is weakly magnetic compared to prior estimates. These observations indicate originates near the at approximately 0.6 orbital radii, rather than primarily from reprocessing on the companion's surface. Relativistic electrons are accelerated in this region, producing fast-cooling with a break at ~200 GHz and a local of ~43 G. The pulsations exhibit a characteristic beat frequency of 1.97 minutes, arising from the near-commensurability between the 's spin period and the binary orbital period of 3.56 hours, which modulates the beam-companion alignment. Observations at 220 GHz show modulation at twice the spin (58.26 s), consistent with emission near the rotating . Double-peaked pulses in the light curve may stem from emission at the two magnetic poles, though the weak field alters beaming interpretations from earlier strong-field models. Polarization observations reveal strong , reaching up to 40% in the optical, with position angles swinging by 180 degrees over a spin cycle, indicative of ordered structuring the emission regions. This polarization pattern, combined with low , supports the origin.

Magnetic field and spin-down

The primary in AR Scorpii possesses a surface estimated at ~15 MG, based on modeling of submillimeter flux densities and emission characteristics from 2025 observations. This weak field strength revises earlier polarimetric estimates of 100–500 MG and classifies the white dwarf as moderately magnetic, without the strong fields typical of polars. The system exhibits no accretion signatures, such as flickering or broad emission lines, with emission powered by the white dwarf's and interaction with the companion. Long-term photometric monitoring spanning nearly seven years has measured a spin-down rate with 50-sigma significance: ν˙=−4.82×10−17\dot{\nu} = -4.82 \times 10^{-17} Hz s−1^{-1}, corresponding to P˙≈3.3×10−13\dot{P} \approx 3.3 \times 10^{-13} s s−1^{-1} and a characteristic age of 5.6 million years. The spin-down luminosity is E˙≈1.5×1033\dot{E} \approx 1.5 \times 10^{33} erg s−1^{-1}, supplying power for the broadband emission. This exceeds the observed by factors of ~10, suggesting low radiative efficiency or additional energy transfer mechanisms. The observed spin-down rate implies a stronger than expected from radiation for a weak field of 15 MG, suggesting contributions from interaction with the red dwarf's wind or , rather than vacuum braking alone. The classical formula, E˙=B2R6Ω4sin⁡2α6c3,\dot{E} = \frac{B^2 R^6 \Omega^4 \sin^2\alpha}{6 c^3}, provides an estimate under assumptions (with R≈5×108R \approx 5 \times 10^8 cm, Ω=2π/P\Omega = 2\pi / P), but does not match the measured E˙\dot{E} without a higher effective B or modified geometry. Applying parameters consistent with the weak field underestimates the spin-down, highlighting the need for non- models in this . Compared to neutron star pulsars, AR Scorpii displays similar relativistic beaming but at lower magnetic field strengths and longer spin periods, resulting in a reduced overall energy scale, though the binary interaction amplifies the observed effects.

Evolutionary aspects

Binary evolution

AR Scorpii is believed to have originated as a post-common envelope binary system, formed from an initial configuration consisting of a main-sequence primary star with a mass of 2–3 M⊙ and a secondary star of approximately 1 M⊙. During the primary's evolution off the main sequence, it expanded into a red giant and initiated unstable mass transfer, leading to a common envelope phase in which the secondary spiraled inward, ejecting the envelope and tightening the orbit. This process resulted in the formation of a white dwarf with a mass around 0.8 M⊙, consistent with standard evolutionary models for such systems. In its current detached state, AR Scorpii features a rapidly rotating magnetic that was likely spun up during earlier accretion episodes following the common envelope ejection, possibly as part of a brief cataclysmic variable phase. The is now undergoing magnetic spin-down, driven by torques from its interaction with the companion's , on a timescale of 1–10 million years. This non-accreting configuration represents a transitional phase in the binary's evolution, where angular momentum loss through gravitational radiation and magnetic braking has not yet resumed significant . Looking ahead, the system's orbital separation is currently too wide for immediate Roche lobe overflow, but continued angular momentum loss could initiate mass transfer in the future, potentially leading to nova outbursts or, if sufficient material accumulates on the white dwarf, a type Ia supernova. The overall system age is estimated at 1–5 Gyr, with the white dwarf's cooling age around 10^8 years, reflecting a mature post-common envelope binary. AR Scorpii is one of the few known non-accreting magnetic white dwarf binaries, serving as a key link between accreting systems like polars and isolated magnetic white dwarfs, with recent surveys identifying around 20-30 such detached magnetic systems among thousands of known white dwarf binaries as of 2024.

Recent changes

A 2023 study analyzing optical light curves of AR Scorpii spanning nine years revealed a secular evolution in the beat pulse amplitudes originating from the white dwarf's magnetic poles. In 2015, the primary beat pulse dominated with an amplitude roughly twice that of the secondary, but by 2023, the two pulses exhibited nearly equal amplitudes, as quantified by the ratio RbeatR_{\rm beat} increasing from 0.42±0.030.42 \pm 0.03 to 0.82−0.85±0.030.82 - 0.85 \pm 0.03. This shift is interpreted as evidence of white dwarf spin-axis precession or possible magnetic field reconfiguration, with a precession cycle estimated at ≥40\geq 40 years. Similar evolution was observed in the linearly polarized flux, where the beat pulse ratio rose from 0.52±0.030.52 \pm 0.03 in 2016 to 0.81±0.030.81 \pm 0.03 in 2023, pointing to changes in the geometry of the emission beams. These alterations suggest dynamic adjustments in how the interacts with the companion star's magnetosphere over short timescales. Very Long Baseline Interferometry (VLBI) conducted in 2023 provided refined measurements of AR Scorpii's position, (π=8.52−0.07+0.04\pi = 8.52^{+0.04}_{-0.07} mas), and (μα=9.48−0.07+0.04\mu_\alpha = 9.48^{+0.04}_{-0.07} mas yr−1^{-1} , μδ=−51.32−0.38+0.22\mu_\delta = -51.32^{+0.22}_{-0.38} mas yr−1^{-1} ), aligning closely with optical data but revealing no evidence of significant . Over the observational baseline, the 's 1.95-minute spin period showed no measurable variation, implying stability in the spin-down rate despite the pulse amplitude changes, though these could hint at underlying variability in the spin-down mechanism. Ongoing photometric monitoring is recommended to capture the full cycle and further probe these short-term dynamics. In 2025, submillimeter observations with the Submillimeter Array at 220 GHz and 345 GHz detected pulsed emission modulated at twice the spin period (58.26 s), confirming emission originating near the at about 0.6 orbital radii. A spectral break at ~200 GHz was identified, and the strength was estimated at approximately 43 MG, suggesting the may be weakly to moderately magnetic (~15 MG), lower than previous estimates of 60-500 MG. These findings refine models of the emission mechanism and magnetic interactions, with implications for the spin-down torque.
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