Starquakes spring stellar surprises

Don Kurtz, Simon Jeffrey and Conny Aerts describe discoveries in the new era of precision asteroseismology. We call it the “Tychonic Principle”: a revolutionary improvement in observational precision inevitably leads to discovery. For Tycho Brahe, the improvement was in precision of astromet- ric position; for us, over the decades since we were students, it has been orders of magnitude improvement in the precision of radial velocity and photometric measure- ments for stars. Three decades ago, stellar radial velocities were measured to 1 kms–1 precision; now, in the best cases they are measured to 10s of cms–1. Three decades ago, stellar light variability was measured to mmag precision (one part per thousand); now in the best cases it is measured to better than µmag precision (one part per million). Stellar astrophysics is being revo- lutionized by this new ultra-high precision. The driving force has been the search for exoplanets. The two main techniques for exoplanet searches – radial velocity and transit measurements – require exquisite precision to detect either the tiny perturba- tive motion of a star being tugged about by a planet, or the slight drop in stellar bright- ness as a planet transits its star. The improvement in radial velocity preci- sion came about from brilliant engineering: 1 Luminosity– effective temperature (Hertzsprung–Russell) diagram showing locations of major pulsating variables coloured roughly by spectral type, the zero- age main sequence and horizontal branch, the Cepheid instability strip, and evolution tracks for model stars of various masses, indicated by small numbers (M⊙). Shadings represent heat-engine p modes (\\\), g modes (///) and strange modes (|||) and acoustically driven stochastic modes (≡). Rough spectral types are shown on the top axis. (Based on figures by J Christensen-Dalsgaard and then by CS Jeffery. See Jeffery & Saio 2016) of stellar apparent brightnesses – the µmag revolution – came with space missions that took photometers above the Earth’s atmos- phere. The highest precision ground-based photometry of one particular star reached 14 µmag – 14 parts per million (Kurtz et al. 2005) – in pulsation amplitude, but typically 1 mmag has been considered old photoelectric photometers, or dozens with CCDs on the ground. The third – and for some purposes the most important – benefit is the nearly continuous observa- tions for four years of about 150000 stars. For decades, groups of astronomers have organized campaigns to observe pulsating stars contemporaneously ground-based spectrographs have been placed in temperature-stabilized vacuums on vibrationally stable platforms with the light from the telescope fibre-fed to the ultra-stable spectrographs. For exoplanet good. With the advent of the French-led ESA CoRoT mis- sion and the NASA Kepler mission, it has become pos- sible to reach µmag precision “Stellar astrophysics is being revolutionized by this new ultra-high precision” from observatories around the world to try to get con- tinuous measurement of the changes in stellar brightness; one project for this is called searches the spectroscopic measurements have to provide true radial velocities to feed into Newton’s form of Kepler’s third law to determine the planets’ masses. This carries its own difficulties; at radial velocity preci- sion better than 1 ms–1 even the definition of radial velocity is interestingly complex (Lindegren & Dravins 2003). But, for astero- seismology, the fundamental data are the pulsation frequencies, with only secondary information coming from the amplitudes of the radial velocity excursions. The improvement in the measurement for thousands of stars simultaneously. The planet hunters have built beautifully stable spectrographs and ultra-precise photometers in their search for exoplanets; we asteroseismologists have used those precision data for new stellar astrophysics. Here, we are primarily showing results from the Kepler mission. For asteroseismol- ogy this mission provided multifold ben- efits over ground-based observations. The obvious one is the µmag precision; another is the observation of 200000 stars simulta- neously, instead of just one at a time with the “Whole Earth Telescope”, (WET; see Provencal et al. 2014). But where WET can observe a single target, or a few targets, for several weeks with duty cycles (fraction of time observing out of the full time possible) of, say, 50%, Kepler observations have bet- ter than 90% duty cycles for four years for 150000 stars. For many asteroseismic tar- gets this unprecedented length of observing time has been the key to discovery. So the planet hunters drove the technol- ogy development. We asteroseismologists have put that technology to excellent use. I

AOD Distributions and Trends of Major Aerosol Species over a Selection of the World's Most Populated Cities Based on the 1st Version of NASA's MERRA Aerosol Reanalysis

NASA recently extended the Modern-Era Retrospective Analysis for Research and Application (MERRA) with an atmospheric aerosol reanalysis which includes five particulate species: sulfate, organic matter, black carbon, mineral dust and sea salt. The MERRA Aerosol Reanalysis (MERRAero) is an innovative tool to study air quality issues around the world for its global and constant coverage and its distinction of aerosol speciation expressed in the form of aerosol optical depth (AOD). The purpose of this manuscript is to apply MERRAero to the study of urban air pollution at the global scale by analyzing the AOD over a period of 13 years (2003-2015) and over a selection of 200 of the world's most populated cities in order to assess the impacts of urbanization, industrialization, air quality regulations and regional transport which affect urban aerosol load. Environmental regulations and the recent global economic recession have helped to decrease the AOD and sulfate aerosols in most cities in North America, Europe and Japan. Rapid industrialization in China over the last two decades resulted in Chinese cities having the highest AOD values in the world. China has nevertheless recently implemented emission control measures which are showing early signs of success in many cities of Southern China where AOD has decreased substantially over the last 13 years. The AOD over South American cities, which is dominated by carbonaceous aerosols, has also decreased over the last decade due to an increase in commodity prices which slowed deforestation activities in the Amazon rainforest. At the opposite, recent urbanization and industrialization in India and Bangladesh resulted in a strong increase of AOD, sulfate and carbonaceous aerosols in most cities of these two countries. The AOD over most cities in Northern Africa and Western Asia changed little over the last decade. Emissions of natural aerosols, which cities in these two regions tend to be mostly composed of, don't tend to fluctuate significantly on an annual basis

Technical Report Series on Global Modeling and Data Assimilation

NASA's Global Modeling and Assimilation Office has extended the Modern-Era Retrospective Analysis for Research and Application (MERRA) tool with five atmospheric aerosol species (sulfates, organic carbon, black carbon, mineral dust and sea salt). This inclusion of aerosol reanalysis data is now known as MERRAero. This study analyses a ten-year period (July 2002 - June 2012) MERRAero aerosol reanalysis applied to the study of aerosol optical depth (AOD) and its trends for the aforementioned aerosol species over the world's major cities (with a population of over 2 million inhabitants). We found that a proportion of various aerosol species in total AOD exhibited a geographical dependence. Cities in industrialized regions (North America, Europe, central and eastern Asia) are characterized by a strong proportion of sulfate aerosols. Organic carbon aerosols are dominant over cities which are located in regions where biomass burning frequently occurs (South America and southern Africa). Mineral dust dominates other aerosol species in cities located in proximity to the major deserts (northern Africa and western Asia). Sea salt aerosols are prominent in coastal cities but are dominant aerosol species in very few of them. AOD trends are declining over cities in North America, Europe and Japan, as a result of effective air quality regulation. By contrast, the economic boom in China and India has led to increasing AOD trends over most cities in these two highly-populated countries. Increasing AOD trends over cities in the Middle East are caused by increasing desert dust

Evaluation of PM2.5 Surface Concentration Simulated by Version 1 of the Nasa's MERRA Aerosol Reanalysis Over Israel and Taiwan

Version 1 of the NASA MERRA Aerosol Reanalysis (MERRAero) assimilates bias-corrected 18 aerosol optical depth (AOD) data from MODIS-Terra and MODIS-Aqua, and simulates particulate 19 matter (PM) concentration data to reproduce a consistent database of AOD and PM concentration around 20 the world from 2002 to the end of 2015. The purpose of this paper is to evaluate MERRAeros simulation 21 of fine PM concentration against surface measurements in two regions of the world with relatively high 22 levels of PM concentration but with profoundly different PM composition, those of Israel and Taiwan. 23 Being surrounded by major deserts, Israels PM load is characterized by a significant contribution of 24 mineral dust, and secondary contributions of sea salt particles, given its proximity to the Mediterranean 25 Sea, and sulfate particles originating from Israels own urban activities and transported from Europe. 26 Taiwans PM load is composed primarily of anthropogenic particles (sulfate, nitrate and carbonaceous 27 particles) locally produced or transported from China, with an additional contribution of springtime 28 transport of mineral dust originating from Chinese and Mongolian deserts. The evaluation in Israel 29 produced favorable results with MERRAero slightly overestimating measurements by 6 on average 30 and reproducing an excellent year-to-year and seasonal fluctuation. The evaluation in Taiwan was less 31 favorable with MERRAero underestimating measurements by 42 on average. Two likely reasons 32 explain this discrepancy: emissions of anthropogenic PM and their precursors are largely uncertain in 33 China, and MERRAero doesnt include nitrate particles in its simulation, a pollutant of predominately 34 anthropogenic sources. MERRAero nevertheless simulates well the concentration of fine PM during the 35 summer, when Taiwan is least affected by the advection of pollution from China

Suppression of X-rays during an optical outburst of the helium dwarf nova KL Dra

KL Dra is a helium accreting AM CVn binary system with an orbital period close to 25 mins. Approximately every 60 days there is a 4 mag optical outburst lasting ~10 days. We present the most sensitive X-ray observations made of an AM CVn system during an outburst cycle. A series of eight observations were made using XMM-Newton which started shortly after the onset of an optical outburst. We find that X-rays are suppressed during the optical outburst. There is some evidence for a spectral evolution of the X-ray spectrum during the course of the outburst. A periodic modulation is seen in the UV data at three epochs -- this is a signature of the binary orbital or the super-hump period. The temperature of the X-ray emitting plasma is cooler compared to dwarf novae, which may suggest a wind is the origin of a significant fraction of the X-ray flux.Comment: Accepted by MNRA

Catching profound optical flares in blazars

Flaring episodes in blazars represent one of the most violent processes observed in extra-galactic objects. Studies of such events shed light on the energetics of the physical processes occurring in the innermost regions of blazars, which cannot otherwise be resolved by any current instruments. In this work, we present some of the largest and most rapid flares captured in the optical band in the blazars 3C 279, OJ 49, S4 0954+658, TXS 1156+295 and PG 1553+113. The source flux was observed to increase by nearly ten times within a timescale of a few weeks. We applied several methods of time series analysis and symmetry analysis. Moreover, we also performed searches for periodicity in the light curves of 3C 279, OJ 49 and PG 1553+113 using the Lomb-Scargle method and found plausible indications of quasi-periodic oscillations (QPOs). In particular, the 33- and 22-day periods found in 3C 279, i.e. a 3:2 ratio, are intriguing. These violent events might originate from magnetohydrodynamical instabilities near the base of the jets, triggered by processes modulated by the magnetic field of the accretion disc. We present a qualitative treatment as the possible explanation for the observed large amplitude flux changes in both the source-intrinsic and source-extrinsic scenarios.Comment: 11 pages, 6 figures, MNRAS accepte

Profound optical flares from the relativistic jets of active galactic nuclei

Intense outbursts in blazars are among the most extreme phenomena seen in extragalactic objects. Studying these events can offer important information about the energetic physical processes taking place within the innermost regions of blazars, which are beyond the resolution of current instruments. This work presents some of the largest and most rapid flares detected in the optical band from the sources 3C 279, OJ 49, S4 0954+658, Ton 599, and PG 1553+113, which are mostly TeV blazars. The source flux increased by nearly ten times within a few weeks, indicating the violent nature of these events. Such energetic events might originate from magnetohydrodynamical instabilities near the base of the jets, triggered by processes modulated by the magnetic field of the accretion disc. We explain the emergence of flares owing to the injection of high-energy particles by the shock wave passing along the relativistic jets. Alternatively, the flares may have also arisen due to geometrical effects related to the jets. We discuss both source-intrinsic and source-extrinsic scenarios as possible explanations for the observed large amplitude flux changes.Comment: 8 pages, 2 figures, 38th International Cosmic Ray Conference (ICRC2023) proceeding

Authenticating the Presence of a Relativistic Massive Black Hole Binary in OJ 287 Using Its General Relativity Centenary Flare : Improved Orbital Parameters

Results from regular monitoring of relativistic compact binaries like PSR 1913+16 are consistent with the dominant (quadrupole) order emission of gravitational waves (GWs). We show that observations associated with the binary black hole (BBH) central engine of blazar OJ 287 demand the inclusion of gravitational radiation reaction effects beyond the quadrupolar order. It turns out that even the effects of certain hereditary contributions to GW emission are required to predict impact flare timings of OJ 287. We develop an approach that incorporates this effect into the BBH model for OJ 287. This allows us to demonstrate an excellent agreement between the observed impact flare timings and those predicted from ten orbital cycles of the BBH central engine model. The deduced rate of orbital period decay is nine orders of magnitude higher than the observed rate in PSR 1913+16, demonstrating again the relativistic nature of OJ 287's central engine. Finally, we argue that precise timing of the predicted 2019 impact flare should allow a test of the celebrated black hole "no-hair theorem" at the 10% level.Peer reviewe

Authenticating the Presence of a Relativistic Massive Black Hole Binary in OJ 287 Using Its General Relativity Centenary Flare: Improved Orbital Parameters

© 2018. The American Astronomical Society. All rights reserved. Results from regular monitoring of relativistic compact binaries like PSR 1913+16 are consistent with the dominant (quadrupole) order emission of gravitational waves (GWs). We show that observations associated with the binary black hole (BBH) central engine of blazar OJ 287 demand the inclusion of gravitational radiation reaction effects beyond the quadrupolar order. It turns out that even the effects of certain hereditary contributions to GW emission are required to predict impact flare timings of OJ 287. We develop an approach that incorporates this effect into the BBH model for OJ 287. This allows us to demonstrate an excellent agreement between the observed impact flare timings and those predicted from ten orbital cycles of the BBH central engine model. The deduced rate of orbital period decay is nine orders of magnitude higher than the observed rate in PSR 1913+16, demonstrating again the relativistic nature of OJ 287's central engine. Finally, we argue that precise timing of the predicted 2019 impact flare should allow a test of the celebrated black hole "no-hair theorem" at the 10% level

Authenticating the Presence of a Relativistic Massive Black Hole Binary in OJ 287 Using Its General Relativity Centenary Flare: Improved Orbital Parameters

Results from regular monitoring of relativistic compact binaries like PSR 1913+16 are consistent with the dominant (quadrupole) order emission of gravitational waves (GWs). We show that observations associated with the binary black hole (BBH) central engine of blazar OJ 287 demand the inclusion of gravitational radiation reaction effects beyond the quadrupolar order. It turns out that even the effects of certain hereditary contributions to GW emission are required to predict impact flare timings of OJ 287. We develop an approach that incorporates this effect into the BBH model for OJ 287. This allows us to demonstrate an excellent agreement between the observed impact flare timings and those predicted from ten orbital cycles of the BBH central engine model. The deduced rate of orbital period decay is nine orders of magnitude higher than the observed rate in PSR 1913+16, demonstrating again the relativistic nature of OJ 287's central engine. Finally, we argue that precise timing of the predicted 2019 impact flare should allow a test of the celebrated black hole "no-hair theorem" at the 10% level