The Astrophysical Journal Letters最新文献_第2页

True Pair-instability Supernova Descendant: Implications for the First Stars’ Mass Distribution 真正的对不稳定超新星后裔：第一代恒星质量分布的含义

The Astrophysical Journal Letters Pub Date : 2024-02-01 DOI: 10.3847/2041-8213/ad2466

I. Koutsouridou, Stefania Salvadori, Á. Skúladóttir

{"title":"True Pair-instability Supernova Descendant: Implications for the First Stars’ Mass Distribution","authors":"I. Koutsouridou, Stefania Salvadori, Á. Skúladóttir","doi":"10.3847/2041-8213/ad2466","DOIUrl":"https://doi.org/10.3847/2041-8213/ad2466","url":null,"abstract":"\u0000 The initial mass function (IMF) of the first Population III (Pop III) stars remains a persistent mystery. Their predicted massive nature implies the existence of stars exploding as pair-instability supernovae (PISNe), but no observational evidence had been found. Now, the LAMOST survey claims to have discovered a pure PISN descendant, J1010+2358, at [Fe/H] = − 2.4. Here we confirm that a massive 250–260 M\u0000 ⊙ PISN is needed to reproduce the abundance pattern of J1010+2358. However, the PISN contribution can be as low as 10%, since key elements are missing to discriminate between scenarios. We investigate the implications of this discovery for the Pop III IMF, by statistical comparison with the predictions of our cosmological galaxy formation model, NEFERTITI. First, we show that the nondetection of mono-enriched PISN descendants at [Fe/H] < − 2.5 allows us to exclude (i) a flat IMF at a 90% confidence level; and (ii) a Larson-type IMF with characteristic mass m\u0000 ch/M\u0000 ⊙ > 191.16x − 132.44, where x is the slope, at a 75% confidence level. Second, we show that if J1010+2358 has only inherited <70% of its metals from a massive PISN, no further constraints can be put on the Pop III IMF. If, instead, J1010+2358 will be confirmed to be a nearly pure (>90%) PISN descendant, it will offer strong and complementary constraints on the Pop III IMF, excluding the steepest and bottom-heaviest IMFs: m\u0000 ch/M\u0000 ⊙ < 143.21x − 225.94. Our work shows that even a single detection of a pure PISN descendant can be crucial to our understanding of the mass distribution of the first stars.","PeriodicalId":507476,"journal":{"name":"The Astrophysical Journal Letters","volume":"53 1-2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139886344","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Measuring Tracers of Planet Formation in the Atmosphere of WASP-77A b: Substellar O/H and C/H Ratios, with a Stellar C/O Ratio and a Potentially Superstellar Ti/H Ratio 测量 WASP-77A b 大气中的行星形成示踪物：亚恒星 O/H 和 C/H 比率，以及恒星 C/O 比率和潜在的超恒星 Ti/H 比率

The Astrophysical Journal Letters Pub Date : 2024-02-01 DOI: 10.3847/2041-8213/ad2000

B. Edwards, Q. Changeat

{"title":"Measuring Tracers of Planet Formation in the Atmosphere of WASP-77A b: Substellar O/H and C/H Ratios, with a Stellar C/O Ratio and a Potentially Superstellar Ti/H Ratio","authors":"B. Edwards, Q. Changeat","doi":"10.3847/2041-8213/ad2000","DOIUrl":"https://doi.org/10.3847/2041-8213/ad2000","url":null,"abstract":"\u0000 We present a comprehensive atmospheric retrieval study of the hot Jupiter WASP-77A b using eclipse observations from the Hubble Space Telescope (HST) and JWST. Using atmospheric retrievals, the spectral features of H2O, CO, and TiO are identified, with volume mixing ratios estimated at log10(VMR) = −4.40\u0000 \u0000\u0000\u0000 \u0000 \u0000 \u0000 \u0000 −\u0000 0.11\u0000 \u0000 \u0000 +\u0000 0.14\u0000 \u0000 \u0000 \u0000 \u0000 , −4.44\u0000 \u0000\u0000\u0000 \u0000 \u0000 \u0000 \u0000 −\u0000 0.28\u0000 \u0000 \u0000 +\u0000 0.34\u0000 \u0000 \u0000 \u0000 \u0000 , and −6.40\u0000 \u0000\u0000\u0000 \u0000 \u0000 \u0000 \u0000 −\u0000 0.23\u0000 \u0000 \u0000 +\u0000 0.22\u0000 \u0000 \u0000 \u0000 \u0000 , respectively. We derive the atmospheric C-to-O ratio—a key planetary formation tracer—to be C/O = 0.54 ± 0.12, which is consistent with both the stellar host value and previous studies of the planet’s atmosphere, suggesting a relatively close-in formation. Computing other elemental ratios (i.e., C/H, O/H, and Ti/H), we conclude that the general enrichment of the atmosphere (i.e., metallicity) is substellar, depleted in C and O, but that Ti appears slightly superstellar. A low C and O content could be obtained, in combination with a stellar C/O ratio if the planet formed outside of the CO2 snow line before migrating inwards. Meanwhile, a superstellar Ti/H could be obtained by late contamination from refractory rich planetesimals. While broadly in agreement with previous works, we do find some differences and discuss these while also highlighting the need for homogeneous analyses when comparative exoplanetology is conducted.","PeriodicalId":507476,"journal":{"name":"The Astrophysical Journal Letters","volume":"26 3-4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139880556","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The Progenitor and Central Engine of a Peculiar GRB 230307A 奇特 GRB 230307A 的祖先和中心引擎

The Astrophysical Journal Letters Pub Date : 2024-02-01 DOI: 10.3847/2041-8213/ad22e2

ZhaoWei Du, H. Lü, Yong Yuan, Xing Yang, E. Liang

{"title":"The Progenitor and Central Engine of a Peculiar GRB 230307A","authors":"ZhaoWei Du, H. Lü, Yong Yuan, Xing Yang, E. Liang","doi":"10.3847/2041-8213/ad22e2","DOIUrl":"https://doi.org/10.3847/2041-8213/ad22e2","url":null,"abstract":"\u0000 Recently, a lack of supernova-associated with long-duration gamma-ray burst (GRB 230307A) at such a low redshift z = 0.065, but associated with a possible kilonova emission, has attracted great attention. Its heavy element nucleosynthesis and the characteristic of soft X-ray emission suggest that the central engine of GRB 230307A is a magnetar that is originated from a binary compact star merger. The calculated lower value of ε ∼ 0.05 suggests that GRB 230307A seems to have an ambiguous progenitor. The lower value of f\u0000 eff = 1.23 implies that GRB 230307A is not likely to be from the effect of “tip of iceberg.” We adopt the magnetar central engine model to fit the observed soft X-ray emission with varying efficiency and find that the parameter constraints of the magnetar falls into a reasonable range, i.e., B < 9.4 × 1015 G and P < 2.5 ms for Γsat = 103, and B < 3.6 × 1015 G and P < 1.05 ms for Γsat = 104. Whether the progenitor of GBR 230307A is from the mergers of neutron star–white dwarf (NS–WD) or neutron star–neutron star (NS–NS) remains unknown. The difference of GW radiation between NS–NS merger and NS–WD merger may be a probe to distinguish the progenitor of GRB 230307A-like events in the future.","PeriodicalId":507476,"journal":{"name":"The Astrophysical Journal Letters","volume":"68 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139817038","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Passing Stars as an Important Driver of Paleoclimate and the Solar System’s Orbital Evolution 过路恒星是古气候和太阳系轨道演变的重要驱动力

The Astrophysical Journal Letters Pub Date : 2024-02-01 DOI: 10.3847/2041-8213/ad24fb

N. Kaib, S. Raymond

{"title":"Passing Stars as an Important Driver of Paleoclimate and the Solar System’s Orbital Evolution","authors":"N. Kaib, S. Raymond","doi":"10.3847/2041-8213/ad24fb","DOIUrl":"https://doi.org/10.3847/2041-8213/ad24fb","url":null,"abstract":"\u0000 Reconstructions of the paleoclimate indicate that ancient climatic fluctuations on Earth are often correlated with variations in its orbital elements. However, the chaos inherent in the solar system’s orbital evolution prevents numerical simulations from confidently predicting Earth’s past orbital evolution beyond 50–100 Myr. Gravitational interactions among the Sun’s planets and asteroids are believed to set this limiting time horizon, but most prior works approximate the solar system as an isolated system and neglect our surrounding Galaxy. Here we present simulations that include the Sun’s nearby stellar population, and we find that close-passing field stars alter our entire planetary system’s orbital evolution via their gravitational perturbations on the giant planets. This shortens the timespan over which Earth’s orbital evolution can be definitively known by a further ∼10%. In particular, in simulations that include an exceptionally close passage of the Sun-like star HD 7977 2.8 Myr ago, new sequences of Earth’s orbital evolution become possible in epochs before ∼50 Myr ago, which includes the Paleocene–Eocene Thermal Maximum. Thus, simulations predicting Earth’s past orbital evolution before ∼50 Myr ago must consider the additional uncertainty from passing stars, which can open new regimes of past orbital evolution not seen in previous modeling efforts.","PeriodicalId":507476,"journal":{"name":"The Astrophysical Journal Letters","volume":"15 9","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139873523","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Three-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASE CHASE 探测到的太阳灯丝爆发的三维速度场

The Astrophysical Journal Letters Pub Date : 2024-01-25 DOI: 10.3847/2041-8213/ad1e4f

Ye Qiu, Chuan Li, Yang Guo, Zhen Li, M. Ding, Linggao Kong

{"title":"Three-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASE","authors":"Ye Qiu, Chuan Li, Yang Guo, Zhen Li, M. Ding, Linggao Kong","doi":"10.3847/2041-8213/ad1e4f","DOIUrl":"https://doi.org/10.3847/2041-8213/ad1e4f","url":null,"abstract":"\u0000 The eruption of solar filaments, also known as prominences appearing off limb, is a common phenomenon in the solar atmosphere. It ejects massive plasma and high-energy particles into interplanetary space, disturbing the solar-terrestrial environment. It is vital to obtain the three-dimensional velocity fields of erupting filaments for space-weather predictions. We derive the three-dimensional kinematics of an off-limb prominence and an on-disk filament, respectively, using the full-disk spectral and imaging data detected by the Chinese Hα Solar Explorer (CHASE). It is found that both the prominence and the filament experience a fast semicircle-shaped expansion at first. The prominence keeps propagating outward with an increasing velocity until escaping successfully, with the south leg of the prominence finally moving back to the Sun in a swirling manner. For the filament, the internal plasma falls back to the Sun in a counterclockwise rotation in the late ejection, matching the failed eruption without a coronal mass ejection. During the eruptions, both the prominence and the filament show material splitting along the line-of-sight direction, revealed by the bimodal Hα spectral profiles. For the prominence, the splitting begins at the top and gradually spreads to almost the whole prominence with a fast blueshift component and a slow redshift component. The material splitting in the filament is more fragmental. As shown by the present results, the CHASE full-disk spectroscopic observations make it possible to systematically study the three-dimensional kinematics of solar filament eruptions.","PeriodicalId":507476,"journal":{"name":"The Astrophysical Journal Letters","volume":"24 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139598497","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

SuNeRF: 3D Reconstruction of the Solar EUV Corona Using Neural Radiance Fields SuNeRF：利用神经辐射场三维重建太阳极紫外冕

The Astrophysical Journal Letters Pub Date : 2024-01-23 DOI: 10.3847/2041-8213/ad12d2

R. Jarolim, Benoit Tremblay, A. Muñoz-Jaramillo, Kyriaki-Margarita Bintsi, A. Jungbluth, Miraflor Santos, A. Vourlidas, J. Mason, Sairam Sundaresan, Cooper Downs, R. Caplan

{"title":"SuNeRF: 3D Reconstruction of the Solar EUV Corona Using Neural Radiance Fields","authors":"R. Jarolim, Benoit Tremblay, A. Muñoz-Jaramillo, Kyriaki-Margarita Bintsi, A. Jungbluth, Miraflor Santos, A. Vourlidas, J. Mason, Sairam Sundaresan, Cooper Downs, R. Caplan","doi":"10.3847/2041-8213/ad12d2","DOIUrl":"https://doi.org/10.3847/2041-8213/ad12d2","url":null,"abstract":"\u0000 To understand its evolution and the effects of its eruptive events, the Sun is permanently monitored by multiple satellite missions. The optically thin emission of the solar plasma and the limited number of viewpoints make it challenging to reconstruct the geometry and structure of the solar atmosphere; however, this information is the missing link to understand the Sun as it is: a 3D evolving star. We present a method that enables a complete 3D representation of the uppermost solar layer (corona) observed in extreme ultraviolet (EUV) light. We use a deep-learning approach for 3D scene representation that accounts for radiative transfer to map the entire solar atmosphere from three simultaneous observations. We demonstrate that our approach provides unprecedented reconstructions of the solar poles and directly enables height estimates of coronal structures, solar filaments, coronal hole profiles, and coronal mass ejections. We validate the approach using model-generated synthetic EUV images, finding that our method accurately captures the 3D geometry of the Sun even from a limited number of 32 ecliptic viewpoints (∣latitude∣ ≤ 7°). We quantify the uncertainties of our model using an ensemble approach that allows us to estimate the model performance in the absence of a ground truth. Our method enables a novel view of our closest star and is a breakthrough technology for the efficient use of multi-instrument data sets, which paves the way for future cluster missions.","PeriodicalId":507476,"journal":{"name":"The Astrophysical Journal Letters","volume":"133 3","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139605196","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The Radial Interplanetary Field Strength at Sunspot Minimum as Polar Field Proxy and Solar Cycle Predictor 太阳黑子极小值时的径向行星际场强作为极地场代用指标和太阳周期预测指标

The Astrophysical Journal Letters Pub Date : 2024-01-22 DOI: 10.3847/2041-8213/ad1c65

Y.-M. Wang

{"title":"The Radial Interplanetary Field Strength at Sunspot Minimum as Polar Field Proxy and Solar Cycle Predictor","authors":"Y.-M. Wang","doi":"10.3847/2041-8213/ad1c65","DOIUrl":"https://doi.org/10.3847/2041-8213/ad1c65","url":null,"abstract":"\u0000 The minimum value of the geomagnetic aa index has served as a remarkably successful predictor of solar cycle amplitude. This value is reached near or just after sunspot minimum, when both the near-Earth solar wind speed and interplanetary magnetic field (IMF) strength fall to their lowest values. At this time, the heliospheric current sheet is flattened toward the heliographic equator and the dominant source of the IMF is the Sun’s axial dipole moment, which, in turn, has its source in the polar fields. As recognized previously, the success of \u0000 \u0000\u0000\u0000 \u0000 \u0000 \u0000 aa\u0000 \u0000 \u0000 min\u0000 \u0000 \u0000 \u0000 \u0000 as solar cycle precursor provides support for dynamo models in which the sunspots of a given cycle are produced by winding up the poloidal field built up during the previous cycle. Because they are highly concentrated toward the poles by the surface meridional flow, the polar fields are difficult to measure reliably. Here we point out that the observed value of the radial IMF strength at solar minimum can be used to constrain the polar field measurements, and that this parameter, which is directly proportional to the Sun’s axial dipole strength, may be an even better solar cycle predictor than geomagnetic activity.","PeriodicalId":507476,"journal":{"name":"The Astrophysical Journal Letters","volume":"42 19","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139608602","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The Link between Nonthermal Velocity and Free Magnetic Energy in Solar Flares 太阳耀斑中的非热速度与自由磁能之间的联系

The Astrophysical Journal Letters Pub Date : 2024-01-15 DOI: 10.3847/2041-8213/ad1bee

James McKevitt, R. Jarolim, Sarah Matthews, Deb Baker, M. Temmer, A. Veronig, Hamish Reid, Lucie M. Green

引用次数: 0

First Observational Evidence for an Interconnected Evolution between Time Lag and QPO Frequency among AGNs AGN 时滞与 QPO 频率之间相互关联演变的首个观测证据

The Astrophysical Journal Letters Pub Date : 2024-01-10 DOI: 10.3847/2041-8213/ad1bf2

Ruisong Xia, Hao Liu, Yongquan Xue

{"title":"First Observational Evidence for an Interconnected Evolution between Time Lag and QPO Frequency among AGNs","authors":"Ruisong Xia, Hao Liu, Yongquan Xue","doi":"10.3847/2041-8213/ad1bf2","DOIUrl":"https://doi.org/10.3847/2041-8213/ad1bf2","url":null,"abstract":"\u0000 Quasiperiodic oscillations (QPOs) have been widely observed in black hole X-ray binaries (BHBs), which often exhibit significant X-ray variations. Extensive research has explored the long-term evolution of the properties of QPOs in BHBs. In contrast, such evolution in active galactic nuclei (AGNs) has remained largely unexplored due to limited observational data. By using the 10 new XMM-Newton observations for the narrow-line Seyfert 1 galaxy RE J1034 + 396 from publicly available data, we analyze the characteristics of its X-ray QPOs and examine their long-term evolution. The hard-band (1–4 keV) QPOs are found in all 10 observations and the frequency of these QPOs evolves ranging at (2.47–2.83) × 10−4 Hz. Furthermore, QPO signals in the soft (0.3–1 keV) and hard bands exhibit strong coherence, although, at times, the variations in the soft band lead those in the hard band (the hard-lag mode), while at other times, it is the reverse (the soft-lag mode). The observations presented here serendipitously captured two ongoing lag reversals between these two modes within about two weeks, which are first seen in RE J1034 + 396 and also among all AGNs. A transition in QPO frequency also takes place within a two-week timeframe, two weeks prior to its corresponding lag reversal, indicating a possible coherence between the transitions of QPO frequency and lag mode with delay. The diagram of time lag versus QPO frequency clearly evidences this interconnected evolution with hysteresis, which is, for the first time, observed among AGNs.","PeriodicalId":507476,"journal":{"name":"The Astrophysical Journal Letters","volume":" 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139627324","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The ALMA-QUARKS Survey: Detection of Two Extremely Dense Substructures in a Massive Prestellar Core ALMA-QUARKS巡天：探测到大质量前恒星核心中的两个极致密子结构

The Astrophysical Journal Letters Pub Date : 2024-01-09 DOI: 10.3847/2041-8213/ad19c3

Xiaofeng Mai, Tie Liu, Xunchuan Liu, Lei Zhu, Guido Garay, Paul F. Goldsmith, M. Juvela, Hongli Liu, E. Mannfors, A. Tej, P. Sanhueza, Shan-Shan Li, F. Xu, Enrique Vázquez Semadeni, Wenyu Jiao, Yaping Peng, T. Baug, Aiyuan Yang, Lokesh Dewangan, L. Bronfman, Gilberto C. G'omez, A. Palau, Chang-Won Lee, Sheng-Li Qin, K. Tatematsu, J. Chibueze, Dongting Yang, Xing Lu, Q. Luo, Q. Gu, Namitha Issac, Suinan Zhang, P. Li, Bo Zhang, L. V. T'oth

{"title":"The ALMA-QUARKS Survey: Detection of Two Extremely Dense Substructures in a Massive Prestellar Core","authors":"Xiaofeng Mai, Tie Liu, Xunchuan Liu, Lei Zhu, Guido Garay, Paul F. Goldsmith, M. Juvela, Hongli Liu, E. Mannfors, A. Tej, P. Sanhueza, Shan-Shan Li, F. Xu, Enrique Vázquez Semadeni, Wenyu Jiao, Yaping Peng, T. Baug, Aiyuan Yang, Lokesh Dewangan, L. Bronfman, Gilberto C. G'omez, A. Palau, Chang-Won Lee, Sheng-Li Qin, K. Tatematsu, J. Chibueze, Dongting Yang, Xing Lu, Q. Luo, Q. Gu, Namitha Issac, Suinan Zhang, P. Li, Bo Zhang, L. V. T'oth","doi":"10.3847/2041-8213/ad19c3","DOIUrl":"https://doi.org/10.3847/2041-8213/ad19c3","url":null,"abstract":"\u0000 Only a handful of massive starless core candidates have been discovered so far, but none of them have been fully confirmed. Within the MM1 clump in the filamentary infrared dark cloud G34.43+0.24 that was covered by the Atacama Large Millimeter/submillimeter Array (ALMA) ATOMS survey at Band 3 (∼2″, 6000 au) and the ALMA-QUARKS survey at Band 6 (∼0.″3, 900 au), two prestellar core candidates MM1-C and E1 with masses of 71 and 20 M\u0000 ⊙ and radii of 2100–4400 au were discovered. The two cores show no obvious sign of star formation activities. In particular, MM1-C is a very promising massive prestellar core candidate with a total gas mass of 71 M\u0000 ⊙. Within MM1-C, we detected two extremely dense substructures, C1 and C2, as characterized by their high densities of \u0000 \u0000\u0000\u0000 \u0000 \u0000 \u0000 n\u0000 \u0000 \u0000 \u0000 \u0000 H\u0000 \u0000 \u0000 2\u0000 \u0000 \u0000 \u0000 \u0000 ∼\u0000 \u0000 \u0000 10\u0000 \u0000 \u0000 8\u0000 –\u0000 9\u0000 \u0000 \u0000 \u0000 \u0000 \u0000 cm\u0000 \u0000 \u0000 −\u0000 3\u0000 \u0000 \u0000 \u0000 \u0000 . Moreover, evidence of further fragmentation in C2 was also revealed. We have detected the primordial fragmentation in the earliest stage of massive star formation, and we speculate that MM1-C would be the birthplace of a massive multiple system. However, we cannot fully rule out the possibility that the massive prestellar core MM1-C will just form a cluster of low-mass stars if it undergoes further fragmentation.","PeriodicalId":507476,"journal":{"name":"The Astrophysical Journal Letters","volume":"12 s2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139628795","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0