The Astrophysical Journal Letters最新文献_第9页

Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes 爱丁顿包络：抛物线轨道上被超大质量黑洞潮汐破坏的恒星的命运

The Astrophysical Journal Letters Pub Date : 2024-08-19 DOI: 10.3847/2041-8213/ad6862

Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato and Yuri Levin

引用次数: 0

Toward Spectrum Coexistence: First Demonstration of the Effectiveness of Boresight Avoidance between the NRAO Green Bank Telescope and Starlink Satellites 实现频谱共存：首次展示 NRAO 绿岸望远镜和 Starlink 卫星之间的同轴回避的有效性

The Astrophysical Journal Letters Pub Date : 2024-08-18 DOI: 10.3847/2041-8213/ad6b24

Bang D. Nhan, Christopher G. De Pree, Matt Iverson, Brenne Gregory, Daniel Dueri, Anthony Beasley and Brian Schepis

{"title":"Toward Spectrum Coexistence: First Demonstration of the Effectiveness of Boresight Avoidance between the NRAO Green Bank Telescope and Starlink Satellites","authors":"Bang D. Nhan, Christopher G. De Pree, Matt Iverson, Brenne Gregory, Daniel Dueri, Anthony Beasley and Brian Schepis","doi":"10.3847/2041-8213/ad6b24","DOIUrl":"https://doi.org/10.3847/2041-8213/ad6b24","url":null,"abstract":"NRAO and SpaceX have been engaged in coordinated testing efforts since Fall 2021, including conducting experiments on different interference avoidance schemes for the Karl G. Jansky Very Large Array in New Mexico, and the Green Bank Telescope (GBT) inside the National Radio Quiet Zone in West Virginia. The Starlink system is capable of avoiding direct illumination of telescope sites with their adaptive tasking to place downlink beams far away. Nevertheless, even satellites operating in this mode can potentially present strong signals into the telescope’s receiver system if they pass close to the telescope’s main beam at the boresight. For additional protection, Starlink satellites can either momentarily redirect or completely disable their downlink channels while they pass within some minimum angular separation threshold from the telescope’s boresight, methods that are referred to as “telescope boresight avoidance.” In two separate experiments conducted since Fall 2023, NRAO and SpaceX arranged to have the GBT observe a fixed R.A./decl. position in the sky, chosen to have a large number of close-to-boresight Starlink passages. Preliminary analysis from these two experiments illustrates the feasibility of these avoidance methods to significantly reduce, if not eliminate, the negative impact of close-to-boresight satellite passages. Importantly, these experiments demonstrate the value of continuing cooperative efforts between NRAO and SpaceX, and expanding cooperation between the radio astronomy and satellite communities more generally.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142013774","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

Can Solar Limb Flare Prediction Be Properly Made by Extreme-ultraviolet Intensities? 能否通过极端紫外线强度正确预测太阳边缘耀斑？

The Astrophysical Journal Letters Pub Date : 2024-08-18 DOI: 10.3847/2041-8213/ad6b9b

Jaewon Lee, Yong-Jae Moon, Hyun-Jin Jeong, Kangwoo Yi and Harim Lee

{"title":"Can Solar Limb Flare Prediction Be Properly Made by Extreme-ultraviolet Intensities?","authors":"Jaewon Lee, Yong-Jae Moon, Hyun-Jin Jeong, Kangwoo Yi and Harim Lee","doi":"10.3847/2041-8213/ad6b9b","DOIUrl":"https://doi.org/10.3847/2041-8213/ad6b9b","url":null,"abstract":"We address the question of whether the solar limb flare prediction can be properly made by EUV intensity, which has less projection effects than solar white light and magnetogram data. We develop empirical and multilayer perceptron (MLP) models to forecast the probability of a major solar limb flare within a day. We use Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) 94 and 131 Å that have high correlations and large slopes with X-ray flare fluxes from 2010 to 2022. We select 240 flares stronger than or equal to the M1.0 class and located near the limb region (60° or more in heliographic longitude). For input data, we use the limb intensity as the sum of SDO/AIA intensities in the limb region and the total intensity of the whole image. We compare the model performances using metrics such as the receiver operating characteristic—area under the curve. Our major results are as follows. First, we can forecast major solar limb flare occurrences with only SDO/AIA 94 and/or 131 Å intensities. Second, our models show better probability prediction than the climatological model. Third, both empirical (AUC = 0.85) and MLP (AUC = 0.84) models have similar performances, which are much better than a random forecast (AUC = 0.50). Finally, it is interesting to note that our model can forecast the flaring probability of all 52 events during the test period, while the models in the NASA/CCMC flare scoreboard can forecast only 22 events. From the above results, we can answer that the solar limb flare prediction using EUV intensity can be properly made.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142013776","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

Chemical Mapping of Temperate Sub-Neptune Atmospheres: Constraining the Deep Interior H2O/H2 Ratio from the Atmospheric CO2/CH4 Ratio 温带海王星下大气化学图谱：从大气中的 CO2/CH4 比率推断内部深处的 H2O/H2 比率

The Astrophysical Journal Letters Pub Date : 2024-08-18 DOI: 10.3847/2041-8213/ad6b25

Jeehyun Yang and Renyu Hu

{"title":"Chemical Mapping of Temperate Sub-Neptune Atmospheres: Constraining the Deep Interior H2O/H2 Ratio from the Atmospheric CO2/CH4 Ratio","authors":"Jeehyun Yang and Renyu Hu","doi":"10.3847/2041-8213/ad6b25","DOIUrl":"https://doi.org/10.3847/2041-8213/ad6b25","url":null,"abstract":"Understanding the planetary envelope composition of sub-Neptune-type exoplanets is challenging due to the inherent degeneracy in their interior composition scenarios. Particularly, the planetary envelope’s H2O/H2 ratio, which can also be expressed as the O/H ratio, provides crucial insights into its original location relative to the ice line during planetary formation. Using self-consistent radiative transfer modeling and a rate-based automatic chemical network generator combined with 1D photochemical kinetic-transport atmospheric modeling, we investigate various atmospheric scenarios of temperate sub-Neptunes, ranging from H2-dominated to H2O-dominated atmospheres with equilibrium temperatures (Teq) of 250—400 K. This study includes examples such as K2-18 b (Teq = 255 K), LP 791-18 c (Teq = 324 K), and TOI-270 d (Teq = 354 K). Our models indicate that the atmospheric CO2/CH4 ratio can be used to infer the deep interior H2O/H2 ratio. Applying this method to recent JWST observations, our findings suggest that K2-18 b likely has an interior that is 50% highly enriched in water, exceeding the water content in a 100 × Z⊙ scenario and suggesting a planetary formation mechanism involving substantial accretion of ices. In contrast, our model suggests that approximately 25% of TOI-270 d’s interior is composed of H2O, which aligns with the conventional metallicity framework with a metallicity higher than 100 × Z⊙. Furthermore, our models identify carbonyl sulfide (OCS) and sulfur dioxide (SO2) as strong indicators for temperate sub-Neptunes with at least 10% of their interior composed of water. These results provide a method to delineate the internal composition and formation mechanisms of temperate sub-Neptunes (Teq < ∼ 500 K) via atmospheric characterization through transmission spectroscopy.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142013785","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

PO and PN in the Envelope of VY Canis Majoris: Elucidating the Chemistry and Origin of Phosphorus VY Canis Majoris包膜中的PO和PN：阐明磷的化学性质和起源

The Astrophysical Journal Letters Pub Date : 2024-08-16 DOI: 10.3847/2041-8213/ad6660

R. Ravi, A. P. Singh, A. M. S. Richards, R. M. Humphreys, L. Decin and L. M. Ziurys

{"title":"PO and PN in the Envelope of VY Canis Majoris: Elucidating the Chemistry and Origin of Phosphorus","authors":"R. Ravi, A. P. Singh, A. M. S. Richards, R. M. Humphreys, L. Decin and L. M. Ziurys","doi":"10.3847/2041-8213/ad6660","DOIUrl":"https://doi.org/10.3847/2041-8213/ad6660","url":null,"abstract":"The J = 5.5 → 4.5 and J = 5 → 4 transitions of PO and PN, respectively, have been imaged in the envelope of hypergiant star VY Canis Majoris (VY CMa) using the Atacama Large Millimeter/submillimeter Array with angular resolutions of 0.″2 and 1.″5 and data from the Submillimeter Telescope of the Arizona Radio Observatory. These maps are the first high-fidelity images of PO and PN in a circumstellar envelope. Both molecules are primarily present in a spherical, star-centered region with a radius ∼60 R* (0.″5), indicating formation by LTE chemistry and then condensation into grains. PN, however, shows additional, fan-shaped emission 2″ southwest of the star, coincident with dust features resolved by Hubble Space Telescope (HST), as well as four newly identified distinct structures 1″–2″ toward the north, east, and west (Cloudlets I–IV), not visible in HST images. The “SW Fan” and the cloudlets are also prominent in the J = 5.5 → 4.5 transition of NS. The correlation of PN with NS, SiO, and dust knots in the SW Fan suggests a formation in shocked gas enhanced with nitrogen. Excess nitrogen is predicted to favor PN synthesis over PO. Abundances for PN and PO in the spherical source are f ∼ 4.4 × 10−8 and 1.4 × 10−7, respectively, relative to H2. Given a cosmic abundance of phosphorus, an unusually high fraction (∼35%) is contained in PO and PN. Alternatively, the stellar winds may be enriched in P (and N) by dredge-up from the interior of VY CMa.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141998709","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

Star Formation by Supernova Implosion 超新星内爆形成恒星

The Astrophysical Journal Letters Pub Date : 2024-08-15 DOI: 10.3847/2041-8213/ad6a57

Leonard E. C. Romano, Andreas Burkert and Manuel Behrendt

{"title":"Star Formation by Supernova Implosion","authors":"Leonard E. C. Romano, Andreas Burkert and Manuel Behrendt","doi":"10.3847/2041-8213/ad6a57","DOIUrl":"https://doi.org/10.3847/2041-8213/ad6a57","url":null,"abstract":"Recent hydrodynamical simulations of the late stages of supernova remnant (SNR) evolution have revealed that as they merge with the ambient medium, SNRs implode, leading to the formation of dense clouds in their center. While being highly chemically enriched by their host SNR, these clouds appear to have similar properties as giant molecular clouds, which are believed to be the main site of star formation. Here, we develop a simple model in order to estimate the efficiency of the star formation that might be triggered by the implosion of SNRs. We separately consider two cases: cyclic star formation, maintained by the episodic driving of feedback from new generations of stars, and a single burst of star formation, triggered by a single explosion. We find that in the cyclic case, star formation is inefficient, with implosion-triggered star formation contributing a few percent of the observed star formation efficiency per freefall timescale. In the single-burst case, higher star formation efficiencies can be obtained. However, while the implosion-triggered process might not contribute much to the overall star formation, due to the high chemical enrichment of the birth clouds, it can explain the formation of a significant fraction of metal-rich stars.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141994401","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

Multiple Subscale Magnetic Reconnection Embedded inside a Heliospheric Current Sheet Reconnection Exhaust: Evidence for Flux Rope Merging 嵌入日光层电流片再连接排气中的多重次尺度磁再连接：通量绳合并的证据

The Astrophysical Journal Letters Pub Date : 2024-08-15 DOI: 10.3847/2041-8213/ad6841

T. D. Phan, J. F. Drake, D. Larson, M. Oieroset, S. Eriksson, Z. Yin, B. Lavraud, M. Swisdak, S. D. Bale, R. Livi, O. Romeo, P. Whittlesey, J. Halekas, A. Rahmati, M. Pulupa, A. Szabo, A. Koval, M. Moncuquet, J. Kasper, M. Stevens, M. Desai and N. Raouafi

{"title":"Multiple Subscale Magnetic Reconnection Embedded inside a Heliospheric Current Sheet Reconnection Exhaust: Evidence for Flux Rope Merging","authors":"T. D. Phan, J. F. Drake, D. Larson, M. Oieroset, S. Eriksson, Z. Yin, B. Lavraud, M. Swisdak, S. D. Bale, R. Livi, O. Romeo, P. Whittlesey, J. Halekas, A. Rahmati, M. Pulupa, A. Szabo, A. Koval, M. Moncuquet, J. Kasper, M. Stevens, M. Desai and N. Raouafi","doi":"10.3847/2041-8213/ad6841","DOIUrl":"https://doi.org/10.3847/2041-8213/ad6841","url":null,"abstract":"We report observations of multiple subscale reconnecting current sheets embedded inside a large-scale heliospheric current sheet (HCS) reconnection exhaust. The discovery was made possible by the unusual skimming trajectory of Parker Solar Probe through a sunward-directed HCS exhaust, sampling structures convecting with the exhaust outflows for more than 3 hr during Encounter 14, at a radial distance of ∼17 solar radii. A large number of subscale current sheets (SCSs) were detected inside the HCS exhaust. Remarkably, five SCSs showed direct evidence for reconnection, displaying near-Alfvénic outflow jets and bifurcated current sheets. The reconnecting SCSs all had small magnetic shears (27°–81°), i.e., strong guide fields. The thickness of the subscale reconnecting current sheets ranged from ∼60 km to ∼5000 km (∼20–2000 ion inertial lengths). The SCS exhausts were directed predominantly in the normal or out-of-plane direction of the HCS, i.e., nearly orthogonal to the HCS exhaust direction. The presence of multiple low-magnetic-shear reconnecting current sheets inside a large-scale exhaust could be associated with coalescence of multiple large flux ropes inside the HCS exhaust. The orientation of some SCS exhausts was partly in the ecliptic plane of the HCS, which may indicate that the coalescence process is highly three-dimensional. Since the coalescence process is likely short-lived, the detection of five such events inside a single HCS crossing could imply the common occurrence of flux rope coalescence in large-scale HCS reconnection exhausts.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141994400","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

Extensive Intrusive Magmatism in the Lunar Farside Apollo and South Pole–Aitken Basins, Chang’e-6 Landing Site 嫦娥六号着陆点月球远侧阿波罗盆地和南极-艾特肯盆地的广泛侵入岩浆活动

The Astrophysical Journal Letters Pub Date : 2024-08-14 DOI: 10.3847/2041-8213/ad698f

Yuqi Qian, James Head, Joseph Michalski, Shengxia Gong, Wei Yang, Zilong Wang, Long Xiao, Xianhua Li and Guochun Zhao

{"title":"Extensive Intrusive Magmatism in the Lunar Farside Apollo and South Pole–Aitken Basins, Chang’e-6 Landing Site","authors":"Yuqi Qian, James Head, Joseph Michalski, Shengxia Gong, Wei Yang, Zilong Wang, Long Xiao, Xianhua Li and Guochun Zhao","doi":"10.3847/2041-8213/ad698f","DOIUrl":"https://doi.org/10.3847/2041-8213/ad698f","url":null,"abstract":"Lunar igneous activities, including intrusive magmatism and extrusive volcanism, and their products contain significant information about the lunar interior and its thermal state. Their distribution is asymmetrical on the nearside and farside, reflecting the global dichotomy. Samples from the South Pole–Aitken (SPA) basin on the farside hold the key to disclosing the dichotomy conundrum and rebalancing the asymmetrical understandings of the Moon, in addition to previously returned nearside samples (Apollo, Luna, Chang’e-5). For the first time, the Chang’e-6 mission obtained ∼1935.5 g of lunar soils from the farside in the southern Apollo basin, northeast of SPA, opening a window to solve this long-standing question. However, compared with the well-known mare/cryptomare volcanism in SPA, intrusive activity has a much more obscure presence and origin, due to its unclear surface expression, thus impeding the ongoing Chang’e-6 sample analysis, which is therefore emphasized here. We found evidence that intrusive magmatism is extensive across SPA, including Mg-suite intrusions, floor-modified craters, and linear/ring dikes, consistent with its intermediate crustal thickness, where dike intrusion is favored. Intrusive magmatism is abundant in the Apollo basin, where Chang’e-6 landed. Two obscure craters were discovered (Apollo X and Q) with evidence for subsurface intrusions, strongly suggesting the intensive intrusion in the region. Plutonic materials are very likely to be obtained by Chang’e-6, especially the Mg-suite from the western peak ring of the Apollo basin that delivered and mixed in the soils by the Chaffee S crater, whose components might provide critical new insights into their petrogenesis, early lunar evolution, and the origin of dichotomy.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141994402","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

A Potential Second Shutoff from AT2018fyk: An Updated Orbital Ephemeris of the Surviving Star under the Repeating Partial Tidal Disruption Event Paradigm AT2018fyk的潜在第二次关闭：重复部分潮汐扰动事件范式下幸存恒星的最新轨道星历表

The Astrophysical Journal Letters Pub Date : 2024-08-13 DOI: 10.3847/2041-8213/ad57b3

Dheeraj Pasham, E. R. Coughlin, M. Guolo, T. Wevers, C. J. Nixon, Jason T. Hinkle and A. Bandopadhyay

{"title":"A Potential Second Shutoff from AT2018fyk: An Updated Orbital Ephemeris of the Surviving Star under the Repeating Partial Tidal Disruption Event Paradigm","authors":"Dheeraj Pasham, E. R. Coughlin, M. Guolo, T. Wevers, C. J. Nixon, Jason T. Hinkle and A. Bandopadhyay","doi":"10.3847/2041-8213/ad57b3","DOIUrl":"https://doi.org/10.3847/2041-8213/ad57b3","url":null,"abstract":"The tidal disruption event (TDE) AT2018fyk showed a rapid dimming event 500 days after discovery, followed by a rebrightening roughly 700 days later. It has been hypothesized that this behavior results from a repeating partial TDE (rpTDE), such that prompt dimmings/shutoffs are coincident with the return of the star to pericenter and rebrightenings generated by the renewed supply of tidally stripped debris. This model predicted that the emission should shut off again around August of 2023. We report AT2018fyk’s continued X-ray and UV monitoring, which shows an X-ray (UV) drop-in flux by a factor of 10 (5) over a span of two months, starting 2023 August 14. This sudden change can be interpreted as the second emission shutoff, which (1) strengthens the rpTDE scenario for AT2018fyk, (2) allows us to constrain the orbital period to a more precise value of 1306 ± 47 days, and (3) establishes that X-ray and UV/optical emission track the fallback rate onto this supermassive black hole—an often-made assumption that otherwise lacks observational verification—and therefore, the UV/optical lightcurve is powered predominantly by processes tied to X-rays. The second cutoff implies that another rebrightening should happen between 2025 May and August, and if the star survived the second encounter, a third shutoff is predicted to occur between 2027 January and July. Finally, low-level accretion from the less-bound debris tail (which is completely unbound/does not contribute to accretion in a nonrepeating TDE) can result in a faint X-ray plateau that could be detectable until the next rebrightening.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141980889","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

Detecting Gravitational-wave Bursts from Black Hole Binaries in the Galactic Center with LISA 用 LISA 探测来自银河中心黑洞双星的引力波爆发

The Astrophysical Journal Letters Pub Date : 2024-08-13 DOI: 10.3847/2041-8213/ad6a10

Alan M. Knee, Jess McIver, Smadar Naoz, Isobel M. Romero-Shaw, Bao-Minh Hoang and Evgeni Grishin

{"title":"Detecting Gravitational-wave Bursts from Black Hole Binaries in the Galactic Center with LISA","authors":"Alan M. Knee, Jess McIver, Smadar Naoz, Isobel M. Romero-Shaw, Bao-Minh Hoang and Evgeni Grishin","doi":"10.3847/2041-8213/ad6a10","DOIUrl":"https://doi.org/10.3847/2041-8213/ad6a10","url":null,"abstract":"Stellar-mass black hole binaries (BHBs) in galactic nuclei are gravitationally perturbed by the central supermassive black hole (SMBH) of the host galaxy, potentially inducing strong eccentricity oscillations through the eccentric Kozai–Lidov mechanism. These highly eccentric binaries emit a train of gravitational-wave (GW) bursts detectable by the Laser Interferometer Space Antenna (LISA)—a planned space-based GW detector—with signal-to-noise ratios up to ∼100 per burst. In this work, we study the GW signature of BHBs orbiting our galaxy’s SMBH, Sgr A*, which are consequently driven to very high eccentricities. We demonstrate that an unmodeled approach using a wavelet decomposition of the data effectively yields the time-frequency properties of each burst, provided that the GW frequency peaks between 10−3 and 10−1 Hz. The wavelet parameters may be used to infer the eccentricity of the binary, measuring within an error of 20%. Our proposed search method can thus constrain the parameter space to be sampled by complementary Bayesian inference methods, which use waveform templates or orthogonal wavelets to reconstruct and subtract the signal from LISA data.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141986378","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