10 research outputs found
Observations Supporting the Role of Magnetoconvection in Energy Supply to the Quiescent Solar Atmosphere
Identifying the two physical mechanisms behind the production and sustenance
of the quiescent solar corona and solar wind poses two of the outstanding
problems in solar physics today. We present analysis of spectroscopic
observations from the Solar and Heliospheric Observatory that are consistent
with a single physical mechanism being responsible for a significant portion of
the heat supplied to the lower solar corona and the initial acceleration of the
solar wind; the ubiquitous action of magnetoconvection-driven reprocessing and
exchange reconnection of the Sun's magnetic field on the supergranular scale.
We deduce that while the net magnetic flux on the scale of a supergranule
controls the injection rate of mass and energy into the transition region
plasma it is the global magnetic topology of the plasma that dictates whether
the released ejecta provides thermal input to the quiet solar corona or becomes
a tributary that feeds the solar wind.Comment: 34 pages, 13 figures - In press Astrophysical Journal (Jan 1 2007
The Post-Eruptive Evolution of a Coronal Dimming
We discuss the post-eruptive evolution of a "coronal dimming" based on
observations of the EUV corona from the Solar and Heliospheric Observatory and
the Transition Region and Coronal Explorer. This discussion highlights the
roles played by magnetoconvection-driven magnetic reconnection and the global
magnetic environment of the plasma in the "filling" and apparent motion of the
region following the eruption of a coronal mass ejection (CME). A crucial
element in our understanding of the dimming region evolution is developed by
monitoring the disappearance and reappearance of bright TRACE "moss" around the
active region giving rise to the CME. We interpret the change in the TRACE moss
as a proxy of the changing coronal magnetic field topology behind the CME
front. We infer that the change in global magnetic topology also results in a
shift of energy balance in the process responsible for the production of the
moss emission while the coronal magnetic topology evolves from closed, to open
and back to closed again because, following the eruption, the moss reforms
around the active region in almost exactly its pre-event configuration. As a
result of the moss evolution, combining our discussion with recent
spectroscopic results of an equatorial coronal hole, we suggest that the
interchangeable use of the term "transient coronal hole" to describe a coronal
dimming is more than just a simple coincidence.Comment: In Press ApJ [May 2007] - 15 pages, 5 figures, 7 movies that are
available upon request [contact author
Simple Magnetic Flux Balance as an Indicator of Neon VIII Doppler Velocity Partitioning in an Equatorial Coronal Hole
We present a novel investigation into the relationship between simple
estimates of magnetic flux balance and the Ne VIII Doppler velocity
partitioning of a large equatorial coronal hole observed by the Solar
Ultraviolet Measurements of Emitted Radiation spectrometer (SUMER) on the Solar
and Heliospheric Observatory (SOHO) in November 1999. We demonstrate that a
considerable fraction of the large scale Doppler velocity pattern in the
coronal hole can be qualitatively described by simple measures of the local
magnetic field conditions, i.e., the relative unbalance of magnetic polarities
and the radial distance required to balance local flux concentrations with
those of opposite polarity.Comment: To appear ApJL (June
Deciphering solar magnetic activity.I. On the relationship between the sunspot cycle and the evolution of small magnetic features
Sunspots are a canonical marker of the Sun's internal magnetic field which flips polarity every similar to 22 yr. The principal variation of sunspots, an similar to 11 yr variation, modulates the amount of the magnetic field that pierces the solar surface and drives significant variations in our star's radiative, particulate, and eruptive output over that period. This paper presents observations from the Solar and Heliospheric Observatory and Solar Dynamics Observatory indicating that the 11 yr sunspot variation is intrinsically tied to the spatio-temporal overlap of the activity bands belonging to the 22 yr magnetic activity cycle. Using a systematic analysis of ubiquitous coronal brightpoints and the magnetic scale on which they appear to form, we show that the landmarks of sunspot cycle 23 can be explained by considering the evolution and interaction of the overlapping activity bands of the longer-scale variability.Astronomy & AstrophysicsSCI(E)[email protected]
Deciphering Solar Magnetic Activity. I. On the Relationship Between the Sunspot Cycle and the Evolution of Small Magnetic Features
Sunspots are a canonical marker of the Sun's internal magnetic field which flips polarity every ~22 yr. The principal variation of sunspots, an ~11 yr variation, modulates the amount of the magnetic field that pierces the solar surface and drives significant variations in our star's radiative, particulate, and eruptive output over that period. This paper presents observations from the Solar and Heliospheric Observatory and Solar Dynamics Observatory indicating that the 11 yr sunspot variation is intrinsically tied to the spatio-temporal overlap of the activity bands belonging to the 22 yr magnetic activity cycle. Using a systematic analysis of ubiquitous coronal brightpoints and the magnetic scale on which they appear to form, we show that the landmarks of sunspot cycle 23 can be explained by considering the evolution and interaction of the overlapping activity bands of the longer-scale variability
Cardiac myosin activation with omecamtiv mecarbil in systolic heart failure
BACKGROUND The selective cardiac myosin activator omecamtiv mecarbil has been shown to improve cardiac function in patients with heart failure with a reduced ejection fraction. Its effect on cardiovascular outcomes is unknown. METHODS We randomly assigned 8256 patients (inpatients and outpatients) with symptomatic chronic heart failure and an ejection fraction of 35% or less to receive omecamtiv mecarbil (using pharmacokinetic-guided doses of 25 mg, 37.5 mg, or 50 mg twice daily) or placebo, in addition to standard heart-failure therapy. The primary outcome was a composite of a first heart-failure event (hospitalization or urgent visit for heart failure) or death from cardiovascular causes. RESULTS During a median of 21.8 months, a primary-outcome event occurred in 1523 of 4120 patients (37.0%) in the omecamtiv mecarbil group and in 1607 of 4112 patients (39.1%) in the placebo group (hazard ratio, 0.92; 95% confidence interval [CI], 0.86 to 0.99; P = 0.03). A total of 808 patients (19.6%) and 798 patients (19.4%), respectively, died from cardiovascular causes (hazard ratio, 1.01; 95% CI, 0.92 to 1.11). There was no significant difference between groups in the change from baseline on the Kansas City Cardiomyopathy Questionnaire total symptom score. At week 24, the change from baseline for the median N-terminal pro-B-type natriuretic peptide level was 10% lower in the omecamtiv mecarbil group than in the placebo group; the median cardiac troponin I level was 4 ng per liter higher. The frequency of cardiac ischemic and ventricular arrhythmia events was similar in the two groups. CONCLUSIONS Among patients with heart failure and a reduced ejection, those who received omecamtiv mecarbil had a lower incidence of a composite of a heart-failure event or death from cardiovascular causes than those who received placebo. (Funded by Amgen and others; GALACTIC-HF ClinicalTrials.gov number, NCT02929329; EudraCT number, 2016 -002299-28.)