If you’ve been following along, you probably already know my frustration (and adventure) in trying to get agenuinereplacementbatteryfor my Samsung Galaxy SIII. Instead of merely letting the sellers “get off”, or pocketing a partially functioning battery, I decided to tear down and document the batteries.
I’ve had several suggestions from friends to buy it from Samsung or contact Samsung directly. The problem was, that Samsung didn’t sell the battery for the SIII on their website. The closest we got was acharger cradle with a batterywhich came up with zero stores where it could be purchased. Thanks Samsung.
I decided to e-mail them via their technical support:
Another One is On The Way!
It seems fourth time is the charm. This time, I decided to go away from all of eBay entirely, and instead spent more atKogan. When you factor in the shipping, the price is similar to that charged by Samsung (AU$42.98 with postage and freight insurance). If it wasn’t genuine, I was going to spew. This is what I got.
With the battery inside another bag, doesn’t really inspire confidence. The rear of the bag had a barcode with HC140111357 and a handwritten I9300 model number.
But a closer look at the markings show they match the genuine battery I already have. The the place of manufacture and assembly matches. The datamatrix barcode encodesGH43-03699A+EB-L1G6LLU+C5ATX12705 in a very similar way to my original encoded GH43-03699A+EB-L1G6LLU+C6NTX04261.
ORIGINAL KOGAN SUPPLIED
Best of all, the NFC antenna was felt under the battery label and functions correctly,however, the battery label itself is a bit smoother and shinier than my original and the Original Accessories hologram sticker is “stuck on top”. There’s also some residual adhesive.
Lately, I’ve been having a few charging issues with my Samsung Galaxy SIII where, despite being connected to the charger, it refuses to completely charge on occasion. There are numerous posts online which claim the problem is in the connector, the cable, the charger and so forth, but I would reckon the problem is actually with my battery. The original battery provided in the phone, once sat flush with the rear of the phone, now sits proud ofthe rear and pushes on the rear plastic shell.
The good old “problem” of swelling lithium-ion cells seems to have reared its head. While the capacity hasn’t reduced too much, it’s a sign that the cell itself is having some internal chemical reactions which may make it somewhat dangerous in the sense that it might vent due to pressure build-up.
It might not look like it from the image on the left, but it’s actually fairly swollen. It’s most obvious when you place it on a flat table and press down on a corner, only to see the opposing corner lift cleanly into the air.
It’s a sign that the battery may be overcharged, or exposed to extreme environmental conditions. I know for a fact, because it’s been with me most of the time, it’s definitely not been “baked” in the sun … so it’s likely that the charging threshold is somehow improperly set, or the cell itself is defective somehow. It’s past its warranty anyway, so it was time to hunt down a new cell.
The market for aftermarket batteries is massive, and many replacements exist, but due to my interests in preserving the NFC functionality of the phone, I decided to opt for a genuine replacement. I found one from a seller nearby, at a good price (not too cheap), and I ordered it.
Over the past year or so there has been a lot of excitement about the release of flexible displays. The mass production of flexible screens is greatly anticipated, in part because of their purported indestructible qualities – but mostly because they guarantee, bona fide, that we are living in the future we imagined as children. In this article, we take a look at flexible screens and displays and give an overview of how they work.
What is a flexible display?
If you haven’t worked it out already, flexible displays are displays which are fully bendable. Samsung announced their line of flexible screens in early 2012, branding them “YOUM” and snapping up other trademarks like FAMOLED (flexible active matrix organic light emitting diode). As Samsung is the world’s largest manufacturer of OLED displays, we expect them to be one of the major players in bringing flexible displays to the market. It’s a very exciting development in screen technology which has a huge number of advantages and extremely cool uses!
How do Flexible Displays work?
The biggest problem getting in the way of making screens flexible was glass. Glass doesn’t bend, it’s thick, heavy and breaks easily. Flexible displays rely largely on existing display technology, known as an OLED (organic light emitting diode) or AMOLED (active matrix light emitting diode) screen.
Traditional AMOLED screens use organic compounds which create their own light source when a current is passed through them. As the OLED pixels create their own light source, they don’t need a back light like LCD screen technology, but the circuitry to control the pixels is fused into glass. Flexible displays simply replace the layers of glass with layers of (flexible) plastic film, allowing for them to be bent and flexed without breaking anything.
Looking to “Corning”, the manufacturers of Gorilla Glass, we can see that a flexible protective glass coating for flexible displays isn’t completely out of the question. Their product Willow Glass will allow for the easy protection of flexible displays.
please follow link to read full article. Very interesting read and technology.
I think it will be the future for all types of visual displays, perhaps even car Dashboards or the table your are working from, the list goes on and on.
The international Rosetta mission was approved in November 1993 as the Planetary Cornerstone Mission in ESA’s long-term space science programme. The mission goal was initially set for a rendezvous with Comet 46 P/Wirtanen. After postponement of the initial launch, a new target was set: Comet 67 P/Churyumov-Gerasimenko. On its 10-year journey to the comet, the spacecraft will also pass by two asteroids.
Rosetta’s main objective is to rendezvous with, and enter orbit around, Comet 67P/Churyumov-Gerasimenko, performing observations of the comet’s nucleus and coma. During the period that Rosetta orbits the comet, 67P/Churyumov-Gerasimenko will reach the closest point to the Sun in its orbit. A lander, named Philae, will be deployed and it will attempt to make the first-ever controlled landing on a comet.
The Rosetta Mission Operations Centre (MOC) is located at ESOC, Darmstadt, Germany.
2 Mar 2004
Ariane 5/Kourou, French Guiana
Highly complex, with 3 Earth & 1 Mars gravity assists en route; On arrival at Comet 67P, Rosetta will orbit the comet, tracking with it toward the Sun
+ Rosetta will track a comet as it arcs toward the Sun and its lander Philae will make the first-ever controlled landing on a comet +
The Flight Control Team
The Flight Control Team (FCT) at ESOC operates from the same Dedicated Control Room (DCR) as Mars Express and Venus Express. Spacecraft Operations Manager (SOM) Andrea Accomazzo, from Italy, oversees a team of four flight control engineers working full-time on Rosetta. The team is further composed by analysts and SPACONs (spacecraft controllers), who support all three ESA interplanetary missions via integrated ground software and daily operations.
Other ESOC teams provide additional support in the areas of Flight Dynamics, Ground Facilities and Software Support.
Mission operations overview
Launch of Ariane-5 flight V138 from the European Space Centre, Kourou, French Guiana, 19 December 2000.
During its 10-year journey to Comet 67P/Churyumov-Gerasimenko, Rosetta will circle the Sun almost four times. It will also cross the asteroid belt twice and gain velocity from gravitational ‘kicks’ provided by close swing-bys of Mars (2007) and Earth (2005, 2007 and 2009).
The launch and early orbit phase (LEOP)
The planned launch date for Rosetta was 07:36:49 UT on 26 February 2004. However, an initial delay due to adverse weather, and a subsequent delay due to a technical issue with the launch vehicle, pushed the launch date back by five days, to 2 March 2004.
After burn-out of the lower stage, the spacecraft and upper stage remained in Earth parking orbit (4000 x 200 km) for about two hours. Ariane’s upper stage then ignited to boost Rosetta into its interplanetary trajectory, before separating from the spacecraft.
Rosetta first travelled away from its home planet, before returning a year after launch, in March 2005. Rosetta then headed to Mars and returned to Earth in November 2007 for its second swing-by of our planet. In November 2009 Rosetta will fly past the Earth for the third and last time to receive the final boost required to reach its final target.
Rosetta alternates periods of active and passive phases during the cruise to Earth. The distance at closest approach is between 300 and 5300 km. Operations are mainly focused on orbit determination for the fundamental swing-by manoeuvres; however payload check-out, calibrations and scientific observations are also performed. If required, orbit correction manoeuvres take place before and after each swing-by.
Animation showing Rosetta’s approach and swingby at Mars
Rosetta flew past Mars in February 2007 at a distance of about 250 km, phasing its trajectory for the next Earth swing-by and, as a spin-off, obtaining some science observations. During the swing-by, Rosetta had to survive an eclipse for which, due to the mission target change, the spacecraft was not specifically designed to handle. This operation required a significant effort by the FCT, but was entirely successful; during the swing-by itself, a communications black-out was also caused by an occultation as the spacecraft passed behind Mars with respect to the Earth.
During the cruise phase, Rosetta alternates between phases of passive and active operation, depending on mission needs. As a secondary scientific objective, Rosetta has observed asteroid Steins in 2008 from a distance of 800 km. In July 2010 only 3160 km will separate Rosetta from asteroid Lutetia when it will fly past. Science data recorded onboard will be transmitted to Earth afterwards.
Following a planned deep-space manoeuvre using the engine to achieve a change in speed of approximately 800 m/s, the spacecraft goes into hibernation between June 2011 and January 2014, due to the very limited power that will be available – which would not allow safe spacecraft operations. Almost all electrical systems are switched off, except for the thermal subsystem, on-board computer, radio receivers, command decoders and power supply.
During this period, Rosetta should record its maximum distance from the Sun, about 800 000 000 km, and Earth, about 1000 000 000 km.
Artist impression-the Rosetta orbiter swoops over the lander soon after touchdown on Comet 67P/Churyumov-Gerasimenko.
In May 2014, Rosetta’s thrusters will brake the spacecraft so that it can match Comet 67P/Churyumov-Gerasimenko’s orbit. The spacecraft will arrive in the comet’s vicinity a few weeks later.
Over the following six months, it will edge closer to the black, dormant nucleus until it is only a few kilometres away. The way will then be clear for the exciting transition to global mapping, lander deployment and the continuing ‘comet chase’ toward the Sun.
The ground station – New Norcia
New Norcia antenna
Since launch, the Rosetta mission has been controlled from a single control centre, the Rosetta Mission Operations Centre (MOC) at ESOC, Darmstadt, using ESA’s DSA 1 deep-space ground station at New Norcia.
During critical mission phases (launch, planet swing-bys, etc.) it is supported for tracking, telemetry and command by other ESA ground stations at Kourou and Cebreros, and by the NASA Deep Space Network (DSN) stations at Madrid, Spain, and Goldstone, USA.
Ground segment & mission control system
This mission uses SCOS-2000
The Rosetta ground segment is designed to meet both the scientific objectives and the challenges imposed by a deep-space mission. These challenges include long turnaround times for signals (up to 100 minutes), low bit rates for data (8 bps), low power availability (it is the first spacecraft ever to fly with solar power generators beyond 3.1 AU from the Sun) and very precise navigation during planetary swing-bys (Rosetta made use of gravity-assist manoeuvres with Mars and Earth to achieve its final orbit around the Sun).
ESOC must cope with the long mission duration and the related problems in scheduling expertise and experienced FCT personnel, while minimising overall cost. The central element of the Rosetta ground segment, the Mission Control System, is based on SCOS-2000.
The Rosetta Science Operations Centre (SOC) will produce detailed scientific mission planning requests, which are submitted to the MOC in the form of operation requests. The SOC will make pre-processed scientific data and the scientific data archive available to the scientific community.
A Rosetta Lander Ground Segment (RLGS) will control the Philae lander, in particular before and after completion of the landing and relay phase. These will be coordinated through the Lander Control Center at the German Aerospace Research Centre (DLR), Cologne, Germany, and the scientific control centre of CNES, France’s space agency, in Toulouse.
The platform and payload
The Rosetta orbiter – spacecraft design
The platformRosetta is a large aluminium box, 2.8 x 2.1 x 2.0 metres in size. The scientific instruments are mounted on the ‘top’ of the box (the Payload Support Module) while the subsystems are on the ‘base’ (Bus Support Module).
On one side of the orbiter is a 2.2m-diameter communications dish antenna – the steerable high-gain antenna; the lander is attached to the opposite face. Two enormous solar panels extend from the other sides. These ‘wings’, each 32 square metres in area, have a total span of about 32m tip-to-tip. Each comprises five panels, and both may be rotated through +/-180° to track the Sun in every attitude assumed by the spacecraft.
In order to investigate the comet nucleus and the gas and dust ejected from the nucleus as the comet approaches the Sun, Rosetta carries a suite of eleven instruments on-board the orbiter; the lander, Philae, is equipped with a further ten instruments to perform surface measurements.
The orbiter instruments combine remote sensing techniques, such as cameras and radio science measurements, with direct sensing systems such as dust and particle analysers. The instruments are provided by collaborative efforts between scientific institutes in ESA member states and the USA. Principal investigators in several European countries and America lead the nationally funded science teams.
Ultraviolet Imaging Spectrometer
Comet Nucleus Sounding Experiment by Radiowave Transmission
Cometary Secondary Ion Mass Analyser
Grain Impact Analyser and Dust Accumulator
Micro-Imaging Dust Analysis System
Microwave Instrument for the Rosetta Orbiter
Optical, Spectroscopic, and Infrared Remote Imaging System
Rosetta Orbiter Spectrometer for Ion and Neutral Analysis
Rosetta Plasma Consortium
Radio Science Investigation
Visible and Infrared Thermal Imaging Spectrometer
Rosetta’s Philae lander on comet nucleus
Lander instrumentsThe ~100-kg Philae lander will be the first spacecraft ever to make a soft landing on the surface of a comet nucleus. The lander is provided by a European consortium under the leadership of the German Aerospace Centre (DLR); other members include ESA, CNES and institutes from Austria, Finland, France, Hungary, Ireland, Italy and the UK. The Philae Lander Control Centre is located at the DLR facility in Cologne, Germany.
The lander structure consists of a baseplate and an instrument platform made in a polygonal sandwich construction, all made of carbon fibre. Some of the instruments and subsystems are beneath a hood that is covered with solar cells.
The lander experiments will study the composition and structure of Comet 67P/Churyumov-Gerasimenko’s nucleus.
Panoramic and microscopic imaging system
Radio sounding, nucleus tomography
Evolved gas analyser – elemental and molecular composition
Evolved gas analyser – isotopic composition
Measurements of surface and subsurface properties
Magnetometer and plasma monitor
Sampling, Drilling and Distribution Subsystem (SD2)
Drilling and sample retrieval
Surface electrical, acoustic and dust impact monitoring