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The NIC is both a physical layer and data link layer device, as it provides physical access to a networking medium and, for IEEE and similar networks, provides a low-level addressing system through the use of MAC addresses that are uniquely assigned to network interfaces.

Network controllers were originally implemented as expansion cards that plugged into a computer bus. The low cost and ubiquity of the Ethernet standard means that most new computers have a network interface controller built into the motherboard.

Newer server motherboards may have multiple network interfaces built-in. The Ethernet capabilities are either integrated into the motherboard chipset or implemented via a low-cost dedicated Ethernet chip.

A separate network card is typically no longer required unless additional independent network connections are needed or some non-Ethernet type of network is used.

A general trend in computer hardware is towards integrating the various components of systems on a chip , and this is also applied to network interface cards.

An Ethernet network controller typically has an 8P8C socket where the network cable is connected. These define a standard receptacle for media-dependent transceivers, so users can easily adapt the network interface to their needs.

LEDs adjacent to or integrated into the network connector inform the user of whether the network is connected, and when data activity occurs.

The NIC may use one or more of the following techniques to indicate the availability of packets to transfer:.

Multiqueue NICs provide multiple transmit and receive queues , allowing packets received by the NIC to be assigned to one of its receive queues.

The NIC may distribute incoming traffic between the receive queues using a hash function. Each receive queue is assigned to a separate interrupt ; by routing each of those interrupts to different CPUs or CPU cores , processing of the interrupt requests triggered by the network traffic received by a single NIC can be distributed improving performance.

The hardware-based distribution of the interrupts, described above, is referred to as receive-side scaling RSS. This technique improves Locality of reference and results in higher overall performance, reduced latency and better hardware utilization because of the higher utilization of CPU caches and fewer required context switches.

With multi-queue NICs, additional performance improvements can be achieved by distributing outgoing traffic among different transmit queues.

By assigning different transmit queues to different CPUs or CPU cores, internal operating system contentions can be avoided.

This approach is usually referred to as transmit packet steering XPS. It is primarily used with high-speed network interfaces, such as Gigabit Ethernet and 10 Gigabit Ethernet, for which the processing overhead of the network stack becomes significant.

Some NICs offer integrated field-programmable gate arrays FPGAs for user-programmable processing of network traffic before it reaches the host computer, allowing for significantly reduced latencies in time-sensitive workloads.

This kind of functionality is usually referred to as user-level networking. From Wikipedia, the free encyclopedia.

Redirected from Solarflare. For the British Rail discount card, see Network Railcard. Not to be confused with network interface device.

A s Ethernet network interface controller card that connects to the motherboard via the now-obsolete ISA bus.

January 7, TechGenix Ltd. Retrieved Network Computing. The same energy releases may produce coronal mass ejections CMEs , although the relationship between CMEs and flares is still not well understood.

X-rays and UV radiation emitted by solar flares can affect Earth's ionosphere and disrupt long-range radio communications.

Direct radio emission at decimetric wavelengths may disturb the operation of radars and other devices that use those frequencies.

Solar flares were first observed on the Sun by Richard Christopher Carrington and independently by Richard Hodgson in [4] as localized visible brightenings of small areas within a sunspot group.

Stellar flares can be inferred by looking at the lightcurves produced from the telescope or satellite data of variety of other stars.

The frequency of occurrence of solar flares varies, from several per day when the Sun is particularly "active" to less than one every week when the Sun is "dormant", following the year cycle the solar cycle.

Large flares are less frequent than smaller ones. Flares occur when accelerated charged particles, mainly electrons, interact with the plasma medium.

Evidence suggests that the phenomenon of magnetic reconnection leads to this copious acceleration of charged particles.

These lines of force quickly reconnect into a lower arcade of loops leaving a helix of magnetic field unconnected to the rest of the arcade.

The sudden release of energy in this reconnection is the origin of the particle acceleration. The unconnected magnetic helical field and the material that it contains may violently expand outwards forming a coronal mass ejection.

Although there is a general agreement on the source of a flare's energy, the mechanisms involved are still not well understood. It's not clear how the magnetic energy is transformed into the kinetic energy of the particles, nor is it known how some particles can be accelerated to the GeV range 10 9 electron volt and beyond.

There are also some inconsistencies regarding the total number of accelerated particles, which sometimes seems to be greater than the total number in the coronal loop.

Scientists are unable to forecast flares. The strength of an event within a class is noted by a numerical suffix ranging from 1 to 9, which is also the factor for that event within the class.

The scheme uses both the intensity and emitting surface. The classification in intensity is qualitative, referring to the flares as: faint f , normal n or brilliant b.

The emitting surface is measured in terms of millionths of the hemisphere and is described below. A flare then is classified taking S or a number that represents its size and a letter that represents its peak intensity, v.

Solar flares strongly influence the local space weather in the vicinity of the Earth. They can produce streams of highly energetic particles in the solar wind or stellar wind , known as a solar particle event.

These particles can impact the Earth's magnetosphere see main article at geomagnetic storm , and present radiation hazards to spacecraft and astronauts.

Additionally, massive solar flares are sometimes accompanied by coronal mass ejections CMEs which can trigger geomagnetic storms that have been known to disable satellites and knock out terrestrial electric power grids for extended periods of time.

The soft X-ray flux of X class flares increases the ionization of the upper atmosphere, which can interfere with short-wave radio communication and can heat the outer atmosphere and thus increase the drag on low orbiting satellites, leading to orbital decay.

Energetic particles in the magnetosphere contribute to the aurora borealis and aurora australis. Energy in the form of hard x-rays can be damaging to spacecraft electronics and are generally the result of large plasma ejection in the upper chromosphere.

The radiation risks posed by solar flares are a major concern in discussions of a human mission to Mars , the Moon, or other planets.

Energetic protons can pass through the human body, causing biochemical damage , [11] presenting a hazard to astronauts during interplanetary travel.

Some kind of physical or magnetic shielding would be required to protect the astronauts. Most proton storms take at least two hours from the time of visual detection to reach Earth's orbit.

A solar flare on January 20, released the highest concentration of protons ever directly measured, [12] giving astronauts as little as 15 minutes to reach shelter.

Flares produce radiation across the electromagnetic spectrum, although with different intensity. They are not very intense in visible light, but they can be very bright at particular atomic lines.

They normally produce bremsstrahlung in X-rays and synchrotron radiation in radio. Richard Carrington observed a flare for the first time on 1 September projecting the image produced by an optical telescope through a broad-band filter.

It was an extraordinarily intense white light flare. Other passband filters are also used. Their discovery did not go public until the end of the conflict.

The same year Southworth also observed the Sun in radio, but as with Hey, his observations were only known after The fast development of radioastronomy revealed new peculiarities of the solar activity like storms and bursts related to the flares.

Today ground-based radiotelescopes observe the Sun from c. Since the beginning of space exploration , telescopes have been sent to space, where they work at wavelengths shorter than UV, which are completely absorbed by the atmosphere, and where flares may be very bright.

Nonetheless, UV observations are today the stars of solar imaging with their incredible fine details that reveal the complexity of the solar corona.

Spacecraft may also bring radio detectors at extremely long wavelengths as long as a few kilometers that cannot propagate through the ionosphere.

In addition to these solar observing facilities, many non-solar astronomical satellites observe flares either intentionally e.

The most powerful flare ever observed was the first one to be observed, [25] on September 1, , and was reported by British astronomer Richard Carrington and independently by an observer named Richard Hodgson.

The event is named the Solar storm of , or the "Carrington event". The flare was visible to a naked eye in white light , and produced stunning auroras down to tropical latitudes such as Cuba or Hawaii, and set telegraph systems on fire.

The ultra-fast coronal mass ejection of August is suspected of triggering magnetic fuses on naval mines during the Vietnam War , and would have been a life-threatening event to Apollo astronauts if it had occurred during a mission to the Moon.

In modern times, the largest solar flare measured with instruments occurred on November 4, This event saturated the GOES detectors, and because of this its classification is only approximate.

Other large solar flares also occurred on April 2, X20 , [35] October 28, X Another X1. The Solar Dynamics Observatory recorded an X9.

On July 23, , a massive, potentially damaging, [ vague ] solar storm solar flare, coronal mass ejection and electromagnetic radiation barely missed Earth.

Flare sprays are a type of eruption associated with solar flares. Current methods of flare prediction are problematic, and there is no certain indication that an active region on the Sun will produce a flare.

However, many properties of sunspots and active regions correlate with flaring. For example, magnetically complex regions based on line-of-sight magnetic field called delta spots produce the largest flares.

A simple scheme of sunspot classification due to McIntosh, or related to fractal complexity [60] is commonly used as a starting point for flare prediction.

The U. From Wikipedia, the free encyclopedia. For the class of stars that undergo similar phenomena, see flare star. For the rose variety, see Rosa 'Sun Flare'.

Play media. Solar flare and its prominence eruption recorded on June 7, by SDO in extreme ultraviolet. Main article: List of solar storms. Solar Physics.

Bibcode : SoPh.. Retrieved May 12, Retrieved May 21, Retrieved 2 June Gordon Cambridge University Press ed.

Archived from the original on Retrieved Retrieved: 18 June Retrieved: 15 July National Geophysical Data Center.

Retrieved 22 December Science NASA. New Scientist. Retrieved 8 April Archived from the original PDF on Retrieved 24 November

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