Pewangi Ruangan Otomatis Stella
By aprillins 15 comments
Beberapa hari yang lalu saya membeli pewangi ruangan di Mirota Kampus untuk kamar saya yang baunya datar-datar saja. Salah satu hal yang membuat kamar saya berbau datar adalah jamur di sisi bawah kasur. Itu jamur bandel banget, sudah dicuci dan dijemur tetap saja baunya begitu. Akhirnya, saya diamkan saja toh tidak mengganggu.
Pertama-tama saya ingat untuk sekedar membeli pewangi ruangan semprot, tetapi karena mata saya melihat alat untuk otomatisasi pewangi ruangan maka saya ambil untuk dilihat terlebih dahulu. Wow, saya kira harganya ratusan ribu ternyata jauh di bawah itu. Pewangi ruangan otomatis bermerek Stella ini harganya Rp56.000-an, sudah termasuk baterai AA dua buah dan garansi 2 hari saja.
Bentuknya Stella
Sayangnya ketika saya tanyakan kepada pramuniaganya, pembelian alat pewangi otomatis itu tidak termasuk spray pewanginya. Spray pewangi itu sendiri, kalau tidak salah, harganya sekitar Rp14.000. Jadi, total yang harus dikeluarkan adalah Rp.70.000. Lumayan juga..
Pewangi ruangan otomatis Stella memiliki timer atau jeda waktu semprot antara lain 10 menit, 20 menit, dan 40 menit. Untuk 10 menit, spray pewangi bisa tahan 15 hari, 20 menit 30 hari, dan 40 menit 60 hari. Namun, secara empiris saya belum membuktikan apakah benar-benar bisa mencapai 60 hari atau tidak.
Stella dibuka
Saya suka dengan pewangi otomatis semacam ini karena tidak perlu repot-repot untuk menyemprotkan sendiri setiap hari. Dulu, saya membeli pewangi semprotan konvensional yang nyatanya membuat saya ingin menyemprotkan setiap hari supaya kamar jadi wangi. Hal tersebut membuat pewangi menjadi cepat habis kurang dari sebulan.
Spray untuk pewangi otomatis ini tersedia dengan wangi apel, jeruk, lemon, dan masih banyak lagi. Silakan dipilih, tetapi saya menyarankan untuk beli yang apel saja karena apel dipercaya sebagai buah yang dapat menghilangkan bau mulut setelah makan. Nah, siapa tahu apel juga bisa menghilangkan bau ruangan yang apek atau tidak sedap menjadi harum. Hehehe.. dicoba saja :mrgreen:
Oh iya, setelah searching di Google ternyata ada juga tuh online shop pewangi otomatis namanya Automatic Parfume, tapi kayaknya alatnya mahal deh soalnya ada yang pakai remote gitu.. keren.. Nih fotonya.
Pewangi Remote
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Minggu, 24 Juli 2011
Minggu, 17 Juli 2011
Uses of Radioisotopes
uses of radioisotopes
Introduction to uses of radioisotopes
Radio Active Isotopes :
Radio active isotopes are also called as Radio isotopes . These are the atoms with different number of neutrons with unstable nucleus . This nucleus decays and emits [alpha] , [beta] , [gamma] rays until isotopes reaches its stability . Once the isotopes reaches its stability , then it becomes totally an another element . Radioactive decay is spontaneous , so its hard to know when it will take place . There are around 3800 radioactive isotopes . There are wide use of radioisotopes.
Isotopes of elements are radioactive are called radioactive isotopes . Because of their radioactivity , their presence or location in a system , and their quantity can be easily determined using radioactivity measuring devices . it is for this reason these find wide application in the industry , medical field , agriculture , chemistry , geology .
Uses of Radioisotopes
A few uses of radioisotopes are listed below :
1. Chemistry : Chemical analysis ( quantitative and qualitative analysis ) and reaction mechanism .
2. Agriculture : Mechanism of plant processes .
3. Medical field : Diagnosis and treatment of diseases .
4. Industry : Detection of flaws in machinery .
5. Geology : Age of rocks and fossils .
Uses of Radio Isotopes in Detail
1. Chemistry :
Chemical analysis : The solubility of sparingly soluble salts such as PbSO4 & AgCl and determination of trace amounts of elements in industrial raw materials & products .
Reaction mechanism : Mechanism of photosynthesis and hydrolysis of esters using 8O18 .
2. Agriculture :
Uptake of phosporous by plants by P32 .
Transport of minerals in plants by S34 .
Irradiation by [gamma] -radiations of seeds to improve yeilds .
3. Medical Field :
Diagnosis and treatment of brain umour by I131 .
Study of restricted circulation of blood by Na24 .
Pumping condition of heart by I131 .
Study of functioning of thyroid gland by I131 .
Detection and treatment of cancer by Co50 and Co60 .
Treatment of blood disorders by Pb32 .
Treatment of thyroid complaints by using I131 .
4. Industry :
Isotopes are used in the selection of correct lubricants .
Isotopes are used in detecting the flaws in the machines .
5. Geology :
Age of fossils ( carbon compounds ) by C14
Age of rocks by U238/ Pb206 radio isotopes .
Related Questions
What are the radioisotopes used for agricultural purposes?
Are all isotopes radioisotopes?
What are the types of radioisotopes?
What are 3 different radioisotopes?
Industrial applications of radioisotopes
Why do scientists measure the half-life of radioisotopes?
Related Pages
Using differentials to approximate
Approximation using differentials
Using chain rule
Using sigma notation
Factorisation using identities
Lcm using venn diagram
Derivative using limits
Using the pythagorean theorem
How to use the substitution method
Terminology used in algebra
*AP and SAT are registered trademarks of the College Board.
About Us | Contact Us | Blog | Homework Help | Teaching Jobs | Search Lessons | Answers
Copyright © 2010 - TutorVista.com, All rights reserved.
Introduction to uses of radioisotopes
Radio Active Isotopes :
Radio active isotopes are also called as Radio isotopes . These are the atoms with different number of neutrons with unstable nucleus . This nucleus decays and emits [alpha] , [beta] , [gamma] rays until isotopes reaches its stability . Once the isotopes reaches its stability , then it becomes totally an another element . Radioactive decay is spontaneous , so its hard to know when it will take place . There are around 3800 radioactive isotopes . There are wide use of radioisotopes.
Isotopes of elements are radioactive are called radioactive isotopes . Because of their radioactivity , their presence or location in a system , and their quantity can be easily determined using radioactivity measuring devices . it is for this reason these find wide application in the industry , medical field , agriculture , chemistry , geology .
Uses of Radioisotopes
A few uses of radioisotopes are listed below :
1. Chemistry : Chemical analysis ( quantitative and qualitative analysis ) and reaction mechanism .
2. Agriculture : Mechanism of plant processes .
3. Medical field : Diagnosis and treatment of diseases .
4. Industry : Detection of flaws in machinery .
5. Geology : Age of rocks and fossils .
Uses of Radio Isotopes in Detail
1. Chemistry :
Chemical analysis : The solubility of sparingly soluble salts such as PbSO4 & AgCl and determination of trace amounts of elements in industrial raw materials & products .
Reaction mechanism : Mechanism of photosynthesis and hydrolysis of esters using 8O18 .
2. Agriculture :
Uptake of phosporous by plants by P32 .
Transport of minerals in plants by S34 .
Irradiation by [gamma] -radiations of seeds to improve yeilds .
3. Medical Field :
Diagnosis and treatment of brain umour by I131 .
Study of restricted circulation of blood by Na24 .
Pumping condition of heart by I131 .
Study of functioning of thyroid gland by I131 .
Detection and treatment of cancer by Co50 and Co60 .
Treatment of blood disorders by Pb32 .
Treatment of thyroid complaints by using I131 .
4. Industry :
Isotopes are used in the selection of correct lubricants .
Isotopes are used in detecting the flaws in the machines .
5. Geology :
Age of fossils ( carbon compounds ) by C14
Age of rocks by U238/ Pb206 radio isotopes .
Related Questions
What are the radioisotopes used for agricultural purposes?
Are all isotopes radioisotopes?
What are the types of radioisotopes?
What are 3 different radioisotopes?
Industrial applications of radioisotopes
Why do scientists measure the half-life of radioisotopes?
Related Pages
Using differentials to approximate
Approximation using differentials
Using chain rule
Using sigma notation
Factorisation using identities
Lcm using venn diagram
Derivative using limits
Using the pythagorean theorem
How to use the substitution method
Terminology used in algebra
*AP and SAT are registered trademarks of the College Board.
About Us | Contact Us | Blog | Homework Help | Teaching Jobs | Search Lessons | Answers
Copyright © 2010 - TutorVista.com, All rights reserved.
Minggu, 03 Juli 2011
Origin of the Elements
Approximately 73% of the mass of the visible universe is in the form of hydrogen. Helium makes up about 25% of the mass, and everything else represents only 2%. While the abundance of these more massive ("heavy", A > 4) elements seems quite low, it is important to remember that most of the atoms in our bodies and Earth are a part of this small portion of the matter of the universe. The low-mass elements, hydrogen and helium, were produced in the hot, dense conditions of the birth of the universe itself. The birth, life, and death of a star is described in terms of nuclear reactions. The chemical elements that make up the matter we observe throughout the universe were created in these reactions.
Approximately 15 billion years ago the universe began as an extremely hot and dense region of radiant energy, the Big Bang. Immediately after its formation, it began to expand and cool. The radiant energy produced quark-antiquarks and electron-positrons, and other particle-antiparticle pairs. However, as the particles and antiparticles collided in the high energy gas, they would annihilate back into electromagnetic energy. As the universe expanded the average energy of the radiation became smaller. Particle creation and annihilation continued until the temperature cooled enough that pair creation became no longer energetically possible.
One of the signatures of the Big Bang that persists today is the long-wavelength radiation that fills the universe. This is radiation left over from the original explosion. The present temperature of this "background" radiation is 2.7 K. (The temperature, T, of a gas or plasma and average particle kinetic energy, E, are related by the Boltzmann constant, k = 1.38 x 10-23 J/K, in the equation E = kT.) Figure 10.1 shows the temperature at various stages in the time evolution of the universe from the quark-gluon plasma to the present time.
Fig. 10-1. The evolution of the universe
At first quarks and electrons had only a fleeting existence as a plasma because the annihilation removed them as fast as they were created. As the universe cooled, the quarks condensed into nucleons. This process was similar to the way steam condenses to liquid droplets as water vapor cools. Further expansion and cooling allowed the neutrons and some of the protons to fuse to helium nuclei. The 73% hydrogen and 25% helium abundances that exists throughout the universe today comes from that condensation period during the first three minutes. The 2% of nuclei more massive than helium present in the universe today were created later in stars.
The nuclear reactions that formed 4He from neutrons and protons were radiative capture reactions. Free neutrons and protons fused to deuterium (d or 2H) with the excess energy emitted as a 2.2 MeV gamma ray,
n + p Æ d + g.
These deuterons could then capture another neutron or free proton to form tritium (3H) or 3He,
d + n Æ 3H + g and d + p Æ 3He + g.
Finally, 4He was produced by the reactions:
d+ d Æ 4He + g, 3He + n Æ 4He + g and 3H + p Æ 4He + g.
Substantial quantities of nuclei more massive than 4He were not made in the Big Bang because the densities and energies of the particles were not great enough to initiate further nuclear reactions.
It took hundreds of thousands of years of further cooling until the average energies of nuclei and electrons were low enough to form stable hydrogen and helium atoms. After about a billion years, clouds of cold atomic hydrogen and helium gas began to be drawn together under the influence of their mutual gravitational forces. The clouds warmed as they contracted to higher densities. When the temperature of the hydrogen gas reached a few million kelvin, nuclear reactions began in the cores of these protostars. Now more massive elements began to be formed in the cores of the very massive stars.
Chapter Contents
The Sun
Other Stars
Books and Articles
last updated: August 9, 2000 webmaster
Approximately 73% of the mass of the visible universe is in the form of hydrogen. Helium makes up about 25% of the mass, and everything else represents only 2%. While the abundance of these more massive ("heavy", A > 4) elements seems quite low, it is important to remember that most of the atoms in our bodies and Earth are a part of this small portion of the matter of the universe. The low-mass elements, hydrogen and helium, were produced in the hot, dense conditions of the birth of the universe itself. The birth, life, and death of a star is described in terms of nuclear reactions. The chemical elements that make up the matter we observe throughout the universe were created in these reactions.
Approximately 15 billion years ago the universe began as an extremely hot and dense region of radiant energy, the Big Bang. Immediately after its formation, it began to expand and cool. The radiant energy produced quark-antiquarks and electron-positrons, and other particle-antiparticle pairs. However, as the particles and antiparticles collided in the high energy gas, they would annihilate back into electromagnetic energy. As the universe expanded the average energy of the radiation became smaller. Particle creation and annihilation continued until the temperature cooled enough that pair creation became no longer energetically possible.
One of the signatures of the Big Bang that persists today is the long-wavelength radiation that fills the universe. This is radiation left over from the original explosion. The present temperature of this "background" radiation is 2.7 K. (The temperature, T, of a gas or plasma and average particle kinetic energy, E, are related by the Boltzmann constant, k = 1.38 x 10-23 J/K, in the equation E = kT.) Figure 10.1 shows the temperature at various stages in the time evolution of the universe from the quark-gluon plasma to the present time.
Fig. 10-1. The evolution of the universe
At first quarks and electrons had only a fleeting existence as a plasma because the annihilation removed them as fast as they were created. As the universe cooled, the quarks condensed into nucleons. This process was similar to the way steam condenses to liquid droplets as water vapor cools. Further expansion and cooling allowed the neutrons and some of the protons to fuse to helium nuclei. The 73% hydrogen and 25% helium abundances that exists throughout the universe today comes from that condensation period during the first three minutes. The 2% of nuclei more massive than helium present in the universe today were created later in stars.
The nuclear reactions that formed 4He from neutrons and protons were radiative capture reactions. Free neutrons and protons fused to deuterium (d or 2H) with the excess energy emitted as a 2.2 MeV gamma ray,
n + p Æ d + g.
These deuterons could then capture another neutron or free proton to form tritium (3H) or 3He,
d + n Æ 3H + g and d + p Æ 3He + g.
Finally, 4He was produced by the reactions:
d+ d Æ 4He + g, 3He + n Æ 4He + g and 3H + p Æ 4He + g.
Substantial quantities of nuclei more massive than 4He were not made in the Big Bang because the densities and energies of the particles were not great enough to initiate further nuclear reactions.
It took hundreds of thousands of years of further cooling until the average energies of nuclei and electrons were low enough to form stable hydrogen and helium atoms. After about a billion years, clouds of cold atomic hydrogen and helium gas began to be drawn together under the influence of their mutual gravitational forces. The clouds warmed as they contracted to higher densities. When the temperature of the hydrogen gas reached a few million kelvin, nuclear reactions began in the cores of these protostars. Now more massive elements began to be formed in the cores of the very massive stars.
Chapter Contents
The Sun
Other Stars
Books and Articles
last updated: August 9, 2000 webmaster
Approximately 15 billion years ago the universe began as an extremely hot and dense region of radiant energy, the Big Bang. Immediately after its formation, it began to expand and cool. The radiant energy produced quark-antiquarks and electron-positrons, and other particle-antiparticle pairs. However, as the particles and antiparticles collided in the high energy gas, they would annihilate back into electromagnetic energy. As the universe expanded the average energy of the radiation became smaller. Particle creation and annihilation continued until the temperature cooled enough that pair creation became no longer energetically possible.
One of the signatures of the Big Bang that persists today is the long-wavelength radiation that fills the universe. This is radiation left over from the original explosion. The present temperature of this "background" radiation is 2.7 K. (The temperature, T, of a gas or plasma and average particle kinetic energy, E, are related by the Boltzmann constant, k = 1.38 x 10-23 J/K, in the equation E = kT.) Figure 10.1 shows the temperature at various stages in the time evolution of the universe from the quark-gluon plasma to the present time.
Fig. 10-1. The evolution of the universe
At first quarks and electrons had only a fleeting existence as a plasma because the annihilation removed them as fast as they were created. As the universe cooled, the quarks condensed into nucleons. This process was similar to the way steam condenses to liquid droplets as water vapor cools. Further expansion and cooling allowed the neutrons and some of the protons to fuse to helium nuclei. The 73% hydrogen and 25% helium abundances that exists throughout the universe today comes from that condensation period during the first three minutes. The 2% of nuclei more massive than helium present in the universe today were created later in stars.
The nuclear reactions that formed 4He from neutrons and protons were radiative capture reactions. Free neutrons and protons fused to deuterium (d or 2H) with the excess energy emitted as a 2.2 MeV gamma ray,
n + p Æ d + g.
These deuterons could then capture another neutron or free proton to form tritium (3H) or 3He,
d + n Æ 3H + g and d + p Æ 3He + g.
Finally, 4He was produced by the reactions:
d+ d Æ 4He + g, 3He + n Æ 4He + g and 3H + p Æ 4He + g.
Substantial quantities of nuclei more massive than 4He were not made in the Big Bang because the densities and energies of the particles were not great enough to initiate further nuclear reactions.
It took hundreds of thousands of years of further cooling until the average energies of nuclei and electrons were low enough to form stable hydrogen and helium atoms. After about a billion years, clouds of cold atomic hydrogen and helium gas began to be drawn together under the influence of their mutual gravitational forces. The clouds warmed as they contracted to higher densities. When the temperature of the hydrogen gas reached a few million kelvin, nuclear reactions began in the cores of these protostars. Now more massive elements began to be formed in the cores of the very massive stars.
Chapter Contents
The Sun
Other Stars
Books and Articles
last updated: August 9, 2000 webmaster
Approximately 73% of the mass of the visible universe is in the form of hydrogen. Helium makes up about 25% of the mass, and everything else represents only 2%. While the abundance of these more massive ("heavy", A > 4) elements seems quite low, it is important to remember that most of the atoms in our bodies and Earth are a part of this small portion of the matter of the universe. The low-mass elements, hydrogen and helium, were produced in the hot, dense conditions of the birth of the universe itself. The birth, life, and death of a star is described in terms of nuclear reactions. The chemical elements that make up the matter we observe throughout the universe were created in these reactions.
Approximately 15 billion years ago the universe began as an extremely hot and dense region of radiant energy, the Big Bang. Immediately after its formation, it began to expand and cool. The radiant energy produced quark-antiquarks and electron-positrons, and other particle-antiparticle pairs. However, as the particles and antiparticles collided in the high energy gas, they would annihilate back into electromagnetic energy. As the universe expanded the average energy of the radiation became smaller. Particle creation and annihilation continued until the temperature cooled enough that pair creation became no longer energetically possible.
One of the signatures of the Big Bang that persists today is the long-wavelength radiation that fills the universe. This is radiation left over from the original explosion. The present temperature of this "background" radiation is 2.7 K. (The temperature, T, of a gas or plasma and average particle kinetic energy, E, are related by the Boltzmann constant, k = 1.38 x 10-23 J/K, in the equation E = kT.) Figure 10.1 shows the temperature at various stages in the time evolution of the universe from the quark-gluon plasma to the present time.
Fig. 10-1. The evolution of the universe
At first quarks and electrons had only a fleeting existence as a plasma because the annihilation removed them as fast as they were created. As the universe cooled, the quarks condensed into nucleons. This process was similar to the way steam condenses to liquid droplets as water vapor cools. Further expansion and cooling allowed the neutrons and some of the protons to fuse to helium nuclei. The 73% hydrogen and 25% helium abundances that exists throughout the universe today comes from that condensation period during the first three minutes. The 2% of nuclei more massive than helium present in the universe today were created later in stars.
The nuclear reactions that formed 4He from neutrons and protons were radiative capture reactions. Free neutrons and protons fused to deuterium (d or 2H) with the excess energy emitted as a 2.2 MeV gamma ray,
n + p Æ d + g.
These deuterons could then capture another neutron or free proton to form tritium (3H) or 3He,
d + n Æ 3H + g and d + p Æ 3He + g.
Finally, 4He was produced by the reactions:
d+ d Æ 4He + g, 3He + n Æ 4He + g and 3H + p Æ 4He + g.
Substantial quantities of nuclei more massive than 4He were not made in the Big Bang because the densities and energies of the particles were not great enough to initiate further nuclear reactions.
It took hundreds of thousands of years of further cooling until the average energies of nuclei and electrons were low enough to form stable hydrogen and helium atoms. After about a billion years, clouds of cold atomic hydrogen and helium gas began to be drawn together under the influence of their mutual gravitational forces. The clouds warmed as they contracted to higher densities. When the temperature of the hydrogen gas reached a few million kelvin, nuclear reactions began in the cores of these protostars. Now more massive elements began to be formed in the cores of the very massive stars.
Chapter Contents
The Sun
Other Stars
Books and Articles
last updated: August 9, 2000 webmaster
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