The star, designated M31-2014-DS1, resided in the neighboring Andromeda Galaxy, situated approximately 2.5 million light-years from Earth. Rather than ending in the typical energetic supernova explosion that disperses stellar material into space, the star’s core imploded quietly to form a black hole, while its outer layers were progressively expelled. This slow, turbulent shedding of stellar material marks a new paradigm in star death scenarios and challenges existing theoretical frameworks.

The research team, led by Kishalay De of the Simons Foundation’s Flatiron Institute, rigorously analyzed observations from NASA’s NEOWISE mission alongside extensive archives from ground- and space-based observatories, compiling a continuous record spanning from 2005 to 2023. In 2014, M31-2014-DS1’s infrared emission began to rise, hinting at changes deep within the star. By 2016, the star’s brightness plummeted within roughly a year, reaching an extraordinary low where it became virtually undetectable in visible and near-infrared wavelengths.

By 2022 and 2023, the star had vanished from the traditional electromagnetic spectrum observable with optical telescopes, dimmed nearly ten thousand times relative to its prime luminosity. Remarkably, residual emission was still detected in mid-infrared wavelengths, albeit at just a tenth of the original brightness. This lingering infrared glow is attributed to dust formed from the ejected stellar material, which absorbs surrounding energy and re-radiates it at longer wavelengths.

The disappearance of M31-2014-DS1 aligns with theoretical models predicting that when massive stars exhaust their nuclear fuel, the gravitational collapse of the core can outpace the explosive power of neutrino-driven shock waves. Typically, neutrino emissions energize a cataclysmic supernova wave strong enough to blow away the outer layers. If this mechanism fails, the outer envelope instead falls inward, augmenting mass accumulation and forcing the birth of a black hole.

The process of black hole formation in this “failed supernova” context has been elusive until now. The data from M31-2014-DS1 provide compelling evidence that only about 1% of the star’s outer gas actually fell into the nascent black hole. Instead, a significant fraction of this convection-driven material enveloped the black hole in a chaotic swirl, reheating and slowly ejecting dust-laden gas observable for decades.

Convection—an internal circulatory mechanism driven by stark temperature gradients between the star’s hot core and cooler outer layers—is central to this behavior. The convective motion stirs the star’s atmosphere, imparting angular momentum to the gas and preventing its direct fall into the black hole. Instead, the gas orbits and interacts dynamically, forming a disk-like structure and powering a gradual outflow that cools and condenses into obscuring dust.

Andrea Antoni, a co-author on the study and a research fellow at Flatiron, emphasized the significance of the convection models: “Unlike a straightforward implosion lasting mere months, the accretion and ejection processes in this context unfold over decades. This brings about sustained brightness in infrared wavelengths as the dusty material persists.” This mechanism explains the slow fading and extended infrared afterglow that characterize these silent black hole births.

Such insights have broader implications for astrophysics. Understanding why some stars explode spectacularly as supernovae while others succumb silently to black holes fills a critical gap in stellar evolution theory. Moreover, these events shape galactic ecology by regulating how heavy elements are recycled and how black holes populate the cosmos.

Reevaluating previous observations of a similar object, NGC 6946-BH1, within this new convection-driven framework revealed parallel evolutionary pathways. Once considered anomalies, these “oddities” may represent a distinct class of stellar death, reinforcing the notion that stellar black hole formation is governed by more complex physics than previously understood.

The longevity of the infrared emission from these events, potentially observable with instruments like the James Webb Space Telescope, offers astronomers a new window into black hole formation. As dust progressively cools and dims, these cosmic beacons provide a persistent signature of a star’s quiet demise over decades, rather than the transient flash of a supernova.

This transformative discovery confirms longstanding theoretical expectations and highlights the exceptional promise of combining archival data with cutting-edge observations. As Kishalay De underscored, “Witnessing a star vanish so completely yet be visible through its dusty aftermath revolutionizes our perspective on the life cycles of massive stars and the birth of black holes.”

Ultimately, M31-2014-DS1 exemplifies the intricate interplay of gravitational collapse, convection-driven gas dynamics, and dust formation processes. It anchors a new narrative in astronomy—one where the darkest endings of stars illuminate our path to understanding the universe’s most enigmatic objects.

Subject of Research: Black hole formation in massive stars through failed supernova collapse.

Article Title: Disappearance of a massive star in the Andromeda Galaxy due to formation of a black hole

News Publication Date: 12-Feb-2026

Web References: http://dx.doi.org/10.1126/science.adt4853

Image Credits: Keith Miller, Caltech/IPAC – SELab

Keywords

Black holes, Stars, Celestial bodies, Space sciences, Astronomy, Astrophysics, Supernovae, Stellar explosions, Solar physics, Stellar dynamics, Stellar evolution, Observational astrophysics, Observational astronomy

The analysis centers around the supernova designated SN2025pht. Detected on June 29, 2025, this cosmic event radiates from NGC 1637, a spiral galaxy situated a remarkable 40 million light-years away from our own planet. Previous explorations in stellar evolution had documented red supergiants — colossal stars characterized by their impressive size and luminous displays — but few have been able to unravel the mystery of why these stars rarely transition into supernovae. The JWST’s keen observational prowess has bridged the gap between theory and reality, revealing that these red supergiants do explode, albeit shrouded within thick clouds of obscuring dust.

As the researchers delved deeper, the dust surrounding SN2025pht opened a Pandora’s box of inquiries. Generally rich in silicates, red supergiants like Betelgeuse have long been studied for their explosive potential post-core collapse. However, the JWST uncovered something unexpected: the dust enveloping SN2025pht contained a significant amount of carbon. This finding suggests a beautiful complexity within supergiant stars, pointing towards their ability to dredge up material from their core in their final moments, thus enriching their surface and altering the composition of circumstellar dust.

The observational study, set to be published on October 8 in The Astrophysical Journal Letters, not only draws attention with its thrilling insights but also represents a pioneering achievement for JWST. In a stunning revelation, researchers have successfully identified a supernova progenitor star, clear evidence of the JWST’s potential to illuminate the domains of stellar death that had remained murky for decades.

The discoveries regarding SN2025pht are monumental, specifically as they correlate with longstanding hypotheses about the luminosity of red supergiants. Astronomers have long speculated that these extraordinary stars should be shining beacons in the night sky, detectable enough to spot before their cataclysmic endings. Yet, this has not been the case until the advent of the JWST. The JWST’s advanced capabilities for infrared observation allowed astronomers to penetrate the dust veil that has previously concealed these stars, leading to a revelation that sheds light on the obscured lives of stars destined for a violent end.

Leading this return to astronomical light is Charlie Kilpatrick from Northwestern University, who expressed deep enthusiasm over the technological capabilities that have allowed scientists to gather quality infrared data that transforms past assumptions. The collaboration with graduate student Aswin Suresh exemplifies the power of interdisciplinary teamwork in cutting-edge research. The duo, alongside their collaborators, is thrumming with excitement as they combine the archival power of the Hubble Space Telescope with JWST’s latest observations, resulting in a comprehensive analysis of SN2025pht’s progenitor star.

The findings suggest that the thick cloak of dust enveloping massive stars may be the reason behind their apparent scarcity in the supernovae record. The JWST’s resolution reveals these stars — while immensely luminous — may remain virtually undetectable due to the surrounding dust. The correlation of mass and dustiness emerges as a new trend that may dramatically alter how astronomers approach the study of stellar evolutions and the mechanics of supernovae explosions.

Significantly, the implications of discovering a carbon-rich progenitor extend well beyond this instance. It introduces the potential for a re-evaluation of our understanding of stellar material composition and its cyclical journey, impacting theories surrounding star formation and supernova events. The shift in comprehension is not merely academic; it resonates throughout the scientific community and could very well lead to renewed methodologies in studying the cosmos at large.

The astronomers reinforce that the recent revelations concerning dust properties not only solve long-kept riddles but also raise further questions about how many more hidden stars similar to SN2025pht await discovery. As the team sets its sights on identifying similar candidates for future explosions, anticipations rise for the capabilities the upcoming Nancy Grace Roman Space Telescope will provide. This innovative instrument is projected to hold the resolution and sensitivity required to catch these elusive stars in varying states as they transition towards their explosive endings.

In sum, the study of SN2025pht not only represents a crucial stepping stone towards elucidating the behaviors of supergiants in their final years but also ushers in a new era of exploration. With instruments like the JWST and Roman Space Telescope at our disposal, the forthcoming decades promise a bounty of discoveries that could redefine our understanding of galaxy evolution, star death, and the intricate tapestry of the universe.

As we transcend the boundaries of traditional astrophysical constraints, the revelations of SN2025pht reaffirm an essential truth: the more we learn about the universe’s stars, the clearer the universe’s mysteries become. This work stands as a testament to the power of modern astronomy, revealing that often, the most profound astronomical discoveries are merely waiting beneath a shroud of dust.

Subject of Research: The Type II SN 2025pht in NGC 1637 and its red supergiant progenitor star
Article Title: The Type II SN 2025pht in NGC 1637: A red supergiant with carbon-rich circumstellar dust as the first JWST detection of a supernova progenitor star
News Publication Date: 8-Oct-2025
Web References: [Not applicable]
References: [Not applicable]
Image Credits: NASA, ESA, CSA, STScI, Charles Kilpatrick (Northwestern), Aswin Suresh (Northwestern)

Keywords

Cosmic Events, James Webb Space Telescope, Supernova Progenitor, NGC 1637, Red Supergiant Star, Astrophysics, Stellar Evolution, Dust Obscuration, Infrared Observations.

For years, astronomers have been puzzled by the detection of what are known as long-period transients (LPTs) in radio waves emanating from our galaxy. Unlike traditional pulsars, which produce radio emissions that last only milliseconds, these new signals exhibit an entirely different pattern, emitting for much longer periods of time. The periodicity of these signals, occurring roughly every 10 to 125 minutes, caught the attention of astronomers, prompting extensive research to understand their origins. The implications of this study extend beyond mere curiosity, as they contribute to our comprehension of stellar evolution and the gravitational dynamics of celestial binaries.

Dr. Iris de Ruiter, leading the research from the University of Amsterdam, now based at the University of Sydney, spearheaded the investigation into these mysterious long-period signals, utilizing novel imaging techniques combined with data from the Low Frequency Array (LOFAR). This international radio telescope acts like a sophisticated camera, allowing researchers to pinpoint the exact location of the radio pulse in the sky. This innovative approach enabled the team to trace the signals to a specific binary star system located approximately 1,600 light-years away, deep in the reaches of the constellation Ursa Major.

Upon further investigation, researchers discovered that the radio emissions were not originating from a single star but rather from a binary system consisting of a white dwarf and a red dwarf. The white dwarf, a remnant of a sun-like star that has expelled its outer layers, orbits the smaller but more numerous red dwarf in a dance of gravitational attraction. This interaction between the two stars is believed to be responsible for the peculiar radio pulses observed, marking a significant shift in our understanding of binary star interactions.

The frequency of the emitted radio bursts is correlated with the orbital period of the two stars, which completes a cycle every 125 minutes. This periodicity offers a clue into the mechanisms generating the radio emissions, with researchers theorizing that they may result from the intense magnetic fields associated with the white dwarf or from the interactions between the magnetic fields of both stars in the binary system. Such interactions could illuminate previously uncharted aspects of stellar behavior and magnetic field evolution, opening new avenues for exploration in astrophysics.

Dr. Kaustubh Rajwade from the University of Oxford emphasized the significance of these findings, noting that they expand our understanding of which types of celestial bodies can emit detectable radio waves. Previously, pulsars, which are the remnants of supernova explosions, were thought to be the only compact objects capable of producing such emissions. This new discovery indicates that white dwarfs, often overlooked in studies of radio emissions, can also contribute to our understanding of astrophysical processes in unique and exciting ways.

Throughout the study, researchers collaborated across various disciplines, integrating insights from different astronomical techniques. This interdisciplinary approach was crucial in piecing together the puzzle of long-period transients, demonstrating the importance of collaboration in scientific discovery. By leveraging multiple observational platforms and analytical methods, the team was able to decipher the complex nature of these radio signals and their relation to binary star systems.

In recent years, approximately ten similar radio-emitting systems have been reported by various research groups. However, confirming whether these pulses originate from a white dwarf or a neutron star has remained elusive. The current study stands out as a landmark contribution, providing compelling evidence that white dwarfs, alongside neutron stars, can produce the characteristic radio emissions observed.

The implications of this research extend beyond mere curiosity about exotic celestial phenomena. As astronomers continue to discover and study long-period transients, they gain deeper insights into the life cycles of stars, their evolution, and the gravitational forces at play in the universe. The unexpected detection of coherent radio emissions from white dwarfs may help astronomers probe the evolving nature of magnetic fields in these stellar remnants, contributing to a more comprehensive understanding of their lifecycle.

Both Dr. de Ruiter and Dr. Rajwade express excitement about the potential for future discoveries in this domain, prioritizing the need for further observations and analyses. As researchers sift through data from the LOFAR telescope, they anticipate uncovering more examples of these long-period transients, each one providing new insights into the extreme astrophysical environments that can create detectable radio emissions.

The discovery heralds a new understanding of the incredible dynamics of binary star systems and their capacity to produce unexpected and complex radio signals. This study not only challenges previous assumptions regarding the sources of radio emissions in space but also paves the way for future research in astrophysics, including the search for new types of celestial phenomena that could reshape our understanding of the universe.

In summary, the discovery of radio pulses from a previously unsuspected binary star system illustrates the complexity and richness of the universe, inviting both awe and curiosity among scientists and the general public alike. As the research community continues to explore these phenomena, it promises to deepen our connection to the cosmos and enhance our understanding of the intricate architecture of the universe.

Subject of Research: Radio Pulses from Binary Star Systems
Article Title: Sporadic radio pulses from a white dwarf binary at the orbital period
News Publication Date: 12-Mar-2025
Web References: https://www.nature.com/articles/s41550-025-02491-0
References: Not applicable
Image Credits: © Daniëlle Futselaar/artsource.nl

Keywords

Long-period transients, binary star systems, radio astronomy, white dwarf, red dwarf, magnetic fields, astrophysics, pulsars.