Flare Intensity Research Articles

Lower Limit of Line Edge Roughness in High-Dose Exposure of Chemically Amplified Extreme Ultraviolet Resists

The line edge roughness (LER) of resist patterns is a critical issue in the high-volume production of semiconductor devices. LER is inversely proportional to the square root of exposure dose. However, LER cannot be reduced below a certain value when exposure dose is increased or when sensitivity is decreased. In this study, the cause of this lower limit was investigated by Monte Carlo simulation. The dependences of the lower limit of LER on acid generator concentration, feature size, optical image contrast, and flare intensity were clarified. The decomposition effect of acid generators during exposure is a dominant factor for the lower limit of LER in the relationship between LER and exposure dose (or sensitivity).

PROPERTIES OF SEQUENTIAL CHROMOSPHERIC BRIGHTENINGS AND ASSOCIATED FLARE RIBBONS

We report on the physical properties of solar sequential chromospheric brightenings (SCBs) observed in conjunction with moderate-sized chromospheric flares with associated CMEs. To characterize these ephemeral events, we developed automated procedures to identify and track subsections (kernels) of solar flares and associated SCBs using high resolution H-alpha images. Following the algorithmic identification and a statistical analysis, we compare and find the following: SCBs are distinctly different from flare kernels in their temporal characteristics of intensity, Doppler structure, duration, and location properties. We demonstrate that flare ribbons are themselves made up of subsections exhibiting differing characteristics. Flare kernels are measured to have a mean propagation speed of 0.2 km/s and a maximum speed of 2.3 km/s over a mean distance of 5 x 10^3 km. Within the studied population of SCBs, different classes of characteristics are observed with coincident negative, positive, or both negative and positive Doppler shifts of a few km/s. The appearance of SCBs precede peak flare intensity by ~12 minutes and decay ~1 hour later. They are also found to propagate laterally away from flare center in clusters at 41 km/s or 89 km/s. Given SCBs distinctive nature compared to flares, we suggest a different physical mechanism relating to their origin than the associated flare. We present a heuristic model of the origin of SCBs.

On the probability of occurrence of extreme space weather events

By virtue of their rarity, extreme space weather events, such as the Carrington event of 1859, are difficult to study, their rates of occurrence are difficult to estimate, and prediction of a specific future event is virtually impossible. Additionally, events may be extreme relative to one parameter but normal relative to others. In this study, we analyze several measures of the severity of space weather events (flare intensity, coronal mass ejection speeds, Dst, and >30 MeV proton fluences as inferred from nitrate records) to estimate the probability of occurrence of extreme events. By showing that the frequency of occurrence scales as an inverse power of the severity of the event, and assuming that this relationship holds at higher magnitudes, we are able to estimate the probability that an event larger than some criteria will occur within a certain interval of time in the future. For example, the probability of another Carrington event (based on Dst < −850 nT) occurring within the next decade is ∼12%. We also identify and address several limitations with this approach. In particular, we assume time stationarity, and thus, the effects of long‐term space climate change are not considered. While this technique cannot be used to predict specific events, it may ultimately be useful for probabilistic forecasting.

INITIATION OF CORONAL MASS EJECTION AND ASSOCIATED FLARE CAUSED BY HELICAL KINK INSTABILITY OBSERVED BYSDO/AIA

In this paper, we present multiwavelength observations of helical kink instability as a trigger of a CME which occurred in AR NOAA 11163 on 24 February 2011. The CME was associated with a M3.5 limb flare. High resolution observations from SDO/AIA suggest the development of helical kink instability in the erupting prominence, which implies a flux rope structure of the magnetic field. A brightening starts below the apex of the prominence with its slow rising motion (~100 km/s) during the activation phase. A bright structure, indicative of a helix with ~3-4 turns, was transiently formed at this position. The corresponding twist of ~$6\pi-8\pi$ is sufficient to generate the helical kink instability in a flux rope according to recently developed models. A slowly rising blob structure was subsequently formed at the apex of the prominence, and a flaring loop was observed near the footpoints. Within two minutes, a second blob was formed in the northern prominence leg. The second blob erupts (like a plasmoid ejection) with the detachment of the northern prominence leg, and flare intensity maximizes. The first blob at the prominence apex shows rotational motion in the counterclockwise direction in the plane of sky, interpreted as unwinding motion of a helix, and it also erupts to give the coronal mass ejection (CME). RHESSI hard X-ray sources show the two footpoint sources and a loop-top source during the flare. We found RHESSI hard X-ray flux, soft X-ray flux derivative and CME acceleration in the low corona correlate well, which is in agreement with the standard flare model (CSHKP). We also discuss the possible role of ballooning as well as torus instabilities in driving the CME. We conclude that the CME and flare were triggered by the helical kink instability in a flux rope and accelerated mainly by the torus instability.

CAN A NANOFLARE MODEL OF EXTREME-ULTRAVIOLET IRRADIANCES DESCRIBE THE HEATING OF THE SOLAR CORONA?

Nanoflares, the basic unit of impulsive energy release may produce much of the solar background emission. Extrapolation of the energy frequency distribution of observed microflares, which follows a power law to lower energies can give an estimation of the importance of nanoflares for heating the solar corona. If the power law index is greater than 2, then the nanoflare contribution is dominant. We model time series of extreme ultraviolet emission radiance, as random flares with a power law exponent of the flare event distribution. The model is based on three key parameters, the flare rate, the flare duration and the power law exponent of the flare intensity frequency distribution. We use this model to simulate emission line radiance detected in 171 \AA, observed by STEREO/EUVI and SDO/AIA. The Observed light curves are matched with simulated light curves using an Artificial Neural Network and parameter values are determined across regions of active region, quiet sun, and coronal hole. The damping rate of nanoflares is compared with radiative losses cooling time. The effect of background emission, data cadence, and network sensitivity on the key parameters of model is studied. Most of the observed light curves have a power law exponent, $\alpha$, greater than the critical value 2. At these sites nanoflare heating could be significant.

Role of Vascular Endothelial Growth Factor in the Breakdown of the Blood-Aqueous Barrier After Retinal Laser Photocoagulation in Pigmented Rabbits

Retinal laser photocoagulation is used to treat a variety of retinal diseases. Breakdown of the blood-aqueous barrier has been noted after retinal laser photocoagulation. The effect of vascular endothelial growth factor (VEGF) on the function of the blood-aqueous barrier after retinal laser photocoagulation remains undetermined. The current study was designed to evaluate the relationship between intraocular levels of VEGF and breakdown of the blood-aqueous barrier after retinal laser photocoagulation in rabbits. Pigmented rabbits were treated with retinal laser photocoagulation in one eye; the other served as control. Laser flare photometry was carried out on post-treatment days 1, 3, 7, and 14. Animals were sacrificed at the time period just mentioned postlaser, the eyes were removed, and samples of vitreous and aqueous humor were collected. Intraocular VEGF levels were measured by using an immunoassay. An intravitreal injection of VEGF was administered, and the aqueous flare intensity and VEGF levels in the aqueous and vitreous humor were measured at the time periods just mentioned. A significant increase in the aqueous flare intensity after retinal laser photocoagulation was noticed on postoperative day 1, with the values returning to baseline levels on day 14. The VEGF levels in the vitreous of the lasered eyes were significantly increased on day 1 compared with the nonlasered control eyes. The VEGF levels in the aqueous humor of the lasered eyes were also significantly increased on day 1 compared with the control eyes. An intravitreal injection of VEGF induced a significant increase in the aqueous flare intensity and VEGF levels in the aqueous and vitreous humor. The current results suggested that retinal laser photocoagulation can produce a breakdown of the blood-aqueous barrier. VEGF may play a role in the blood-aqueous barrier dysfunction after retinal laser photocoagulation.

Discovery in 1960 of the Flare Nimbus Phenomenon and Changes with Time in Its Interpretation

During the International Geophysical Year (IGY, 1957/1958) Dunsink Observatory near Dublin in Ireland was a World Data Centre for Solar Activity. In this circumstance, Hα Lyot Heliograph records secured on a daily basis between 07:00 – 14:00 UT at the Cape of Good Hope (then an integral link in a network of similar instruments contributing during the IGY to global monitoring of solar chromospheric activity) were routinely sent to Dunsink for analysis and dissemination. The investigations carried out at Dunsink on these data resulted, inter alia, in the discovery of the Flare Nimbus phenomenon. The nimbus comprises a dark expanding halo seen in the plage regions around major flares at, or within a few minutes of, the time of flare maximum intensity in Hα light. It reaches its greatest extent about 30 minutes after flare maximum. Its maximum dimensions (estimated visually) lie in the range 2 – 4×105 km and its duration ranges from ∼ 1 – 2 hours. Within the nimbus the striation pattern is either completely destroyed or loses its pre-flare configuration. An account of this phenomenon and its interpretation appeared primarily, although not exclusively, in the locally produced Dunsink Observatory Publications which are not now easily accessible to the world community of solar researchers. Also, at around the time when the nimbus was first identified and recorded in Lyot Heliograph data at several observatories, techniques in solar physics shifted towards high resolution narrow field observations. Under these conditions no further examples of the nimbus were recorded and the subject has remained dormant over several decades. The present paper again places the scientific results obtained with regard to the nimbus in the public domain, together with an account of the evolution within the scientific community of an explanation of this phenomenon. It is suggested here for the first time, in the light of present day data concerning coronal mass ejections (CMEs) and coronal dimming, that the nimbus provides a signature of CME-related reorganization of the magnetic field in the chromosphere (such that the transverse magnetic field component decreases and transforms into the line of sight component as the vector field stretches out). Coronal dimming provides a complementary signature of CME-related mass depletion in the corona.

An Analysis of the Sunspot Groups and Flares of Solar Cycle 23

Designing a statistical solar flare forecasting technique can benefit greatly from knowledge of the flare frequency of occurrence with respect to sunspot groups. This study analyzed sunspot groups and Hα and X-ray flares reported for the period 1997 – 2007. Annual catalogs were constructed, listing the days that numbered sunspot groups were observed (designated sunspot group-days, SSG-Ds) and for each day a record for each associated Hα flare of importance category one or greater and normal or bright brightness and for each X-ray flare of intensity C 5 or higher. The catalogs were then analyzed to produce frequency distributions of SSG-Ds by year, sunspot group class, likelihood of producing at least one flare overall and by sunspot group class, and frequency of occurrence of numbers of flares per day and flare intensity category. Only 3% of SSG-Ds produced a substantial Hα flare and 7% had a significant X-ray flare. We found that mature, complex sunspot groups were more likely than simple sunspot groups to produce a flare, but the latter were more prevalent than the former. More than half of the SSG-Ds with flares had a maximum intensity flare greater than the lowest category (C-class of intensity five and higher). The fact that certain sunspot group classes had flaring probabilities significantly higher than the combined probabilities of the intensity categories when all SSG-Ds were considered suggest that it might be best to first predict the flaring probability. For sunspot groups found likely to flare, a separate diagnosis of maximum flare intensity category appears feasible.

Flare quasi-periodic pulsations with growing periodicity

We conducted a wavelet analysis of the flare intensity variations for the long duration flare on 2005 August 22 observed with the Nobeyama Radioheliograph at frequencies 17 and 34 GHz and with the Ramaty High Energy Solar Spectroscopic Imager at 25‐ 50 keV. We found that the signals contain a well-pronounced periodicity in which the oscillation period grows from 2.5 to 5 min. An analysis of the loop length and plasma temperature evolution during the flare allowed us to interpret the quasi-periodic pulsations in terms of the second standing harmonics of the slow magnetoacoustic mode. This mode can be generated by the initial impulsive energy release and work as a trigger for the repeated energy releases.

Multiwavelength Study of the M8.9/3B Solar Flare from AR NOAA 10960

We present a multi-wavelength analysis of a long duration white-light solar flare (M8.9/3B) event that occurred on 4 June 2007 from NOAA AR 10960. The flare was observed by several spaceborne instruments, namely SOHO/MDI, Hinode/SOT, TRACE and STEREO/SECCHI. The flare was initiated near a small, positive-polarity, satellite sunspot at the centre of the AR, surrounded by opposite-polarity field regions. MDI images of the AR show considerable amount of changes in a small positive-polarity sunspot of delta configuration during the flare event. SOT/G-band (4305 A) images of the sunspot also suggest the rapid evolution of the positive-polarity sunspot with highly twisted penumbral filaments before the flare event, which were oriented in the counterclockwise direction. It shows the change in orientation and also remarkable disappearance of twisted penumbral filaments (~35-40%) and enhancement in umbral area (~45-50%) during the decay phase of the flare. TRACE and SECCHI observations reveal the successive activations of two helical twisted structures associated with this sunspot, and the corresponding brightening in the chromosphere as observed by the time-sequence images of SOT/Ca II H line (3968 A). The secondary-helical twisted structure is found to be associated with the M8.9 flare event. The brightening starts 6-7 min prior to the flare maximum with the appearance of secondary helical-twisted structure. The flare intensity maximizes as this structure moves away from the AR. This twisted flux-tube associated with the flare triggering, is found to be failed in eruption. The location of the flare is found to coincide with the activation site of the helical twisted structures. We conclude that the activations of successive helical twists in the magnetic flux tubes/ropes plays a crucial role in the energy build-up process and triggering of M-class solar flare without a CME.

Solar proton events during the solar cycle 23 and their association with CME parameters

We have studied the solar proton events associated with the coronal mass ejections (CMEs) and flares during the solar cycle 23 (1997–2006) in order to determine what physical parameters of the solar eruptions might control the SPE intensity and time profile. For total 63 SPEs, we found that (1) SPE rise time, duration time and decrease times depend on a CME speed (cc=0.34, 0.48 and 0.48) and (2) a SPE peak intensity depends on an earthward direction parameter of a CME as well as the CME speed and x-ray flare intensity (cc=0.40, 0.31 and 0.37). The SPEs were divided into two groups according to the correlation between the CME earthward direction parameter and the SPE intensity. First group consists of large six SPEs (>10,000 pfu at >10 MeV proton channel of GOES satellite) and shows a very good correlation (cc=0.65) between the SPE peak intensity and the CME earthward direction parameter. Second group has a relatively weak SPE peak intensity and shows no correlation (cc=0.01) between the SPE peak intensity and the CME earthward direction parameter we found that the first group SPEs are associated with a very fast halo CME (>1400 km/s) and most of those are located at disk except for only one case. Especially, large six SPEs have a good correlation with their associated CME earthward direction parameters, implying that these events are produced by ICME-driven shocks. We also found that those six SPEs are associated with the preceding CMEs originated from the same solar source region and a nearby pre-existing helmet streamer. Thus, we speculate that the preceding CME and helmet streamer might provide seed particles for CME-driven shocks and cause a clear separation between two groups.

Blood-aqueous Barrier Function in a Patient With Choroideremia

The purpose was to determine whether there was a breakdown of the blood-aqueous barrier in a patient with choroideremia. A 27-year-old man with typical choroideremia underwent standardized ophthalmo-logical evaluation, including quantitative measurement of aqueous flare intensity, by a laser flare-cell meter. The results showed areas of atrophy of the choriocapillaries and retinal pigment epithelium in the mid-periphery and posterior pole, although not in the macula. Fluorescein angiography showed areas of loss of the choriocapillaries and retinal pigment epithelium. The fovea was spared with a surrounding zone of hy-perfluorescence. Electroretinography showed a subnormal photopic amplitude and extinguished scotopic response. Electrooculography revealed that the light peak/dark trough ratio was reduced. Goldmann perimetry showed constricted peripheral fields. Laser photometry showed an increase in the aqueous flare intensity in both eyes, as compared with normal subjects. We conclude that the function of the blood-aqueous barrier might be affected in patients with choroideremia.

Effect of Intracameral Triamcinolone to Control Inflammation in Rabbit Eyes

Purpose: To investigate the effect of intracameral triamcinolone on the control of inflammation with rupture of the posterior lens capsule during cataract surgery in rabbit eyes. Methods: Twenty rabbit eyes were subjected to experimentally induced rupture of the posterior lens capsule and prolapse of the vitreous body into the anterior chamber. After anterior vitrectomy with and without triamcinolone, aqueous flare was measured with a laser flare meter on days 1, 3, 7, 14 and 28. Results: Vitrectomized eyes with triamcinolone showed a less marked increase in postoperative aqueous flare intensity on days 14 and 28 than did those without triamcinolone (p

태양 주기 23 기간 동안 태양 고에너지 양성자 이벤트와 코로나 물질 방출 사이의 상관관계

We studied the solar proton events (SPEs) associated with coronal mass ejections (CMEs) during the solar cycle 23 (1997-2006). Using 63 SPE dataset, we investigated the relationship among SPE, flare, and CME, and found that (1) SPE rise time and duration time depend on CME speed and the earthward direction parameter of the CME, and (2) the SPE peak intensity depends on CME speed and X-ray Flare intensity. While inspecting the relation between SPE peak intensity and the direction parameter, we found there are two groups: first group consists of large six SPEs (> 10,000 pfu at > 10 MeV proton channel of GOES satellite) and shows strong correlation (cc

ALO-01 (Morphine Sulfate and Naltrexone Hydrochloride) Extended-Release Capsules in the Treatment of Chronic Pain of Osteoarthritis of the Hip or Knee: Pharmacokinetics, Efficacy, and Safety

ALO-01 (EMBEDA [morphine sulfate and naltrexone hydrochloride] extended-release capsules [King Pharmaceuticals, Inc, Bridgewater, NJ]), indicated for chronic moderate-to-severe pain, is designed to release naltrexone upon tampering (eg, by crushing), reducing morphine-induced subjective effects. This multicenter, randomized, double-blind, crossover study assessed pharmacokinetics, efficacy, and safety of ALO-01 and compared them with extended-release morphine sulfate (ERMS, KADIAN [morphine sulfate extended-release] capsules [Actavis US, Morristown, NJ]) in adults (N = 113) with osteoarthritis pain. Study periods included washout until pain flare (intensity > or =5, 0 to 10; 0 = no pain, 10 = worst pain); dose titration with ERMS (20 to 160mg BID); and randomization to 2 (crossover) 14-day treatment periods with ERMS or ALO-01, separated by 7 days of open-label ERMS. Assessments included pharmacokinetics (morphine, naltrexone), pain scores (0 to 10), Western Ontario and McMaster Universities (WOMAC) Osteoarthritis Index; Patient Global Assessment of Medication (1 to 5; poor to excellent). Mean score at pain flare was 7.1. Morphine exposure from both formulations at steady state was similar. Plasma naltrexone concentrations were below limit-of-quantification for most patients and, when present, did not impact pain scores. During treatment, mean pain intensity (day 14: ERMS, 2.4; ALO-01, 2.3, P = .31), WOMAC change-from-baseline (mean pain, physical function, composite scores), and adverse event frequency were similar. ALO-01 and ERMS provided similar relief of osteoarthritis pain. We present data demonstrating that ALO-01 has steady-state morphine exposure, efficacy, and safety similar to marketed ERMS capsules. Results highlight the potential for morphine in ALO-01 to manage moderate-to-severe osteoarthritis pain, while the sequestered naltrexone does not interfere with efficacy.

Mechanical but not painful electrical stimuli trigger TNF alpha release in human skin

Pro-inflammatory cytokines–in particular tumor necrosis factor (TNF)-alpha–play an important role in pain and hyperalgesia. The stimuli inducing TNF-alpha release in humans and the time course of this release are largely unknown. We performed dermal microdialysis in healthy subjects ( n = 36) during three experimental conditions: The first condition (control) was microdialysis without stimulation, the second condition was 30 min of electrical current stimulation (1 Hz, 20 mA, moderately painful), the third condition was 30 min of repetitive mechanical stimulation via an impact stimulator (bullet 0.5 g; velocity 11 m/s, minimally painful). TNF-alpha was quantified in the samples collected at the end of the baseline perfusion (about 1 h of saline perfusion), at the end of stimulation period (exactly 30 min after stimulation commenced) and at the end of the experiment (exactly 90 min after stimulation commenced) using a commercial enzyme-linked immunosorbent assay. The C-fiber-related flare was quantified with a laser-Doppler imager. ANOVA revealed that TNF-alpha levels increased during the eluate sampling period. At 90 min TNF-alpha in the eluate of the mechanical stimulation condition was significantly increased as compared to electrical current or control condition. Flare intensity was highest in the electrical current stimulation condition and only marginally different from control in mechanical stimulation. Our results show that minimal mechanical trauma is sufficient to induce significant TNF-alpha release in the skin. These results may be relevant to the treatment of posttraumatic pain disorders.

Clinical study on bimanual microphacoemulsification and Acri. mart intraocular lens implantation

Objective To evaluate the clinical effectiveness of birnanual microphacoemulsification and Acri. smart intraocular lens implantation. Methods 75 patients （89 eyes ） with age-related cataract were divided into two groups in random. 34 patients （40 eyes） were treated with bimanual microphacoemulsification while other 41 patients （49 eyes） were treated with conventional phaeoe- mulsification. The visual acuity, phacoemulsifieation time, the endothelial cell loss percentage, anterior chamber aqueous protein concentration, astigmatism and operative complications were observed. Results The mean phaco energy of bimanual group （ 12. 34 ± 7.57 ） % was lower than conventional group （ 17. 16 ± 9. 35） %. The uncorrected visual acuity of bimanual group was better than conventional group in 1 day and 1 week after surgery. Flare intensity at 1 day postoperatively was significantly lower in bimanual group than in conventional group（ 19.47 ± 5.28 and 22.86 ± 4. 30 pc/ms, P =0. 015）. The astigmatism of birnanual group （0.78 ± 0.40） D were significantly lower than conventional group（ 1.12 ± 0. 48 ） D. Conclusions The bimanual microphaeoemulsification and Acri. smart intraocular lens implantation are safe and effective which can be performed through a 1.2 mm incison. Key words: phacoemulsification; lenses, intraoeular; cataract; micro-ineision

The First Survey of X‐Ray Flares from Gamma‐Ray Bursts Observed bySwift: Temporal Properties and Morphology

We present the first systematic investigation of the morphological and timing properties of flares in GRBs observed by Swift XRT. We consider a large sample drawn from all GRBs detected by Swift, INTEGRAL, and HETE-2 prior to 2006 January 31, which had an XRT follow-up and which showed significant flaring. Our sample of 33 GRBs includes long and short, at low and high redshift, and a total of 69 flares. The strongest flares occur in the early phases, with a clear anticorrelation between the flare peak intensity and the flare time of occurrence. Fitting each X-ray flare with a Gaussian model, we find that the mean ratio of the width and peak time is --> ? t/t = 0.13 ? 0.10, albeit with a large scatter. Late flares at times >2000 s have long durations, -->? t > 300 s, and can be very energetic compared to the underlying continuum. We further investigated whether there is a clear link between the number of pulses detected in the prompt phase by BAT and the number of X-ray flares detected by XRT, finding no correlation. However, we find that the distribution of intensity ratios between successive BAT prompt pulses and that between successive XRT flares is the same, an indication of a common origin for gamma-ray pulses and X-ray flares. All evidence indicates that flares are indeed related to the workings of the central engine and, in the standard fireball scenario, originate from internal shocks rather than external shocks. While all flares can be explained by long-lasting engine activity, 29/69 flares may also be explained by refreshed shocks. However, 10 can only be explained by prolonged activity of the central engine.

Saturation of Nonthermal Hard X‐Ray Emission in Solar Flares

We consider a number of flares spanning a range of magnitudes over two decades in GOES soft X-ray luminosity and demonstrate an observational confirmation of the saturation of the nonthermal hard X-ray photon flux in large solar flares. Using the unprecedented spectral and spatial resolution of the RHESSI telescope, we find that the integrated photon flux above 20 keV asymptotically approaches a limiting value with increasing flare intensity, suggesting a saturation of the nonthermal photon production for high electron-beam fluxes in flares. This result is strengthened by considering each of the large flares as an aggregation of multiple fiducial energy release events identified using the high spatial resolution of RHESSI. We argue that the saturation of the photon production sets in as a result of the transition from Coulomb collisions to return current ohmic dissipation dominating the energy losses as the flare magnitudes increase.

Psychophysics, Flare, and Neurosecretory Function in Human Pain Models: Capsaicin Versus Electrically Evoked Pain

Intradermal capsaicin injection (CAP) and electrical current stimulation (ES) are analyzed in respect to patterns and test-retest reliability of pain as well as sensory and neurosecretory changes. In 10 healthy subjects, 2x CAP (50 microg) and 2x ES (5 to 30 mA) were applied to the volar forearm. The time period between 2 identical stimulations was about 4 months. Pain ratings, areas of mechanical hyperalgesia, and allodynia were assessed. The intensity of sensory changes was quantified by using quantitative sensory testing. Neurogenic flare was assessed by using laser Doppler imaging. Calcitonin gene-related peptide (CGRP) release was quantified by dermal microdialysis in combination with an enzyme immunoassay. Time course and peak pain ratings were different between CAP and ES. Test-retest correlation was high (r > or = 0.73). Both models induced primary heat hyperalgesia and primary plus secondary pin-prick hyperalgesia. Allodynia occurred in about half of the subjects. Maximum flare sizes did not differ between CAP and ES, but flare intensities were higher for ES. Test-retest correlation was higher for flare sizes than for flare intensity. A significant CGRP release could only be measured after CAP. The different time courses of pain stimulation (CAP: rapidly decaying pain versus ES: pain plateau) led to different peripheral neurosecretory effects but induced similar central plasticity and hyperalgesia. The present study gives a detailed overview of psychophysical and neurosecretory characteristics induced by noxious stimulation with capsaicin and electrical current. We describe differences, similarities, and reproducibility of these human pain models. These data might help to interpret past and future results of human pain studies using experimental pain.