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خود روزگاری کیوں اور کیسے

خودروزگاری کیوں اور کیسے؟
زندگی اللہ تعالیٰ کی ایک نعمت ہے، زندہ رہنے کے لیے انسان کو کئی مراحل سے گزرنا پڑتا ہے۔ کبھی اس کی صغرسنی ہوتی ہے،کبھی عالم شباب ہوتا ہے اور ایک وقت ایسا آتا ہے کہ پیرانہ سالی کا شکار ہوکرداعی اجل کو لبیک کہہ دیتا ہے۔ ان ادوارِ حیات میں زندگی کی بوقلومونیوں سے واسطہ پڑتا ہے۔ کبھی ایسا وقت ہوتا ہے کہ اس کے دستر خوان پرانواع واقسام کے کھانے چنے ہوتے ہیں اورکبھی ایسی بھی گھڑی آتی ہے کی کئی کئی دن معدودے چند لقموں کے علاوہ دستر خوان پرکوئی قابلِ ذکر چیز نہیں ہوتی ۔لیکن ذی شعور انسان کبھی پستی کا شکار نہیں ہوتا۔ ہمہ وقت کدو کاوش کرتا رہتا ہے۔ اور یوں اس کے ایّام زیست کروٹیں بدلتے ہوئے گزر جاتے ہیں۔
انسان کی یہ بات فطرت میں شامل ہے کی وہ اچھے سے اچھے اور بہتر سے بہتر کی تلاش میں سر گرداں رہتا ہے۔ ملک میں اگر روزگار کے مواقع حکومت عوام الناس کے لیے فراہم نہ کر سکے تو بے روزگاری کے منحوس سائے افق پر منڈ لا نا شروع ہو جائیں ، ہر سوغربت ہی غربت دکھائی دے ، قوم کی کثیر تعدادغربت و افلاس کی لکیر سے نیچے زندگی گزارنے پر مجبور ہو جائے اور کوئی پرسان حال نہ ہو اور کسمپرسی کا شکار لوگ اپنی زندگی کے ہاتھوں پریشان ہوں تو پھر بھی ذی فہم و فراست شخص خود روزگاری کے ذریعے اپنے آپ کو اور اپنے معاشرے کے افراد کو غربت و افلاس کی دلدل سے نکالنے میں اہم کردار ادا کر سکتا ہے۔
حدیث نبوی ہے ’’ الکاسب حبیب اللہ ‘‘حلال روزی کمانے والا اللہ تعالیٰ کا دوست ہوتا ہے۔ اس طرح جو شخص بھی مسلمان ہونے کے ناطے کاروبار سے دلچسپی رکھتا ہے، اپنے اہل خانہ کے لیے دن...

تأثير الفقر على حياة الشاعر الجاهلي: دراسة تحليلية

There is no doubt that poverty is one of the major phenomenon which destroys the entity of the human society and it is also one of the obstacles that prevents the ability and talent of humans to create and innovate in a suitable environment, it also causes the ignorance, mental and social tension, and it also desists human being to strengthen his family ties and make well settled position in the society, it affects adversely the life and mind of humans and forced him to commit crimes and violations in the society. We see that this phenomenon has affected the life of pre-Islamic poet and compelled him on raiding and robbery, so in this article we have tried to highlight the impact of poverty on the life of pre-Islamic poet.

3D Simulations of Low-Mass Proto-Stellar Disks With Certain Initial Conditions Using Smoothed Particle Hydro Dynamics

Results of the numerical study on the initial formation stages of low-mass protostellar systems leading to single, binary, triplet, and quadruple protostar systems formation are reported here. In addition to these various types of protostellar objects we also investigate the overall structure formation that takes place within collapsing molecular cores that yield during the course of evolution the spiral structure formation, ring formation, and bar formation under various initial conditions chosen for a rotating solar mass cloud of molecular hydrogen to mimic the states prevailing in star formation regions in our Milky Way galaxy. There have been three key parameters belonging to the initial star forming conditions whose effects on the overall outcome of protostallar systems have been examined. These parameters are the initial thermal state of the prestellar core, the amplitude of azimuthal density perturbation introduced in initially uniform density state of the core, and the impact of the critical density which governs the transition from isothermal to adiabatic thermodynamic behavior of the collapsing core. For protostellar binaries, the separation is determined as a function of the initial thermal state of the core by varying its initial temperature. For this purpose a slightly modified version of the Burkert and Bodenheimer collapse test is taken into consideration. We find that the result is fairly sensitive to both the initial thermal state of the cloud and the initial azimuthal density perturbation’s amplitude A. For A=10 %, variations of only 1 unit Kelvin below 10 K causes a change of up to 100 AU in protobinary separation, while for this small amplitude of perturbation the initial temperatures above 10 K result a single low-mass fragment, instead of a binary, that does not reach even near to the protostellar densities. However, protostellar binaries, do appear if the amplitude of perturbation is enhanced from 10 % to 25 %. A star forming hydrogen gas is normally considered to be initially at 10 K. For structural formation study, we have explored that an oscillation around this normally considered value can be influential in determining the fate of a collapsing gas as it evolves in its structural properties that may lead to formation of proto-stars. We examined the initial range of temperature of star forming gas between 8 K to 12 K and tried to compare the emerging physical properties within the early phase of formation of protostellar system. According to our findings the spiral structures are likely to appear in a strongly perturbed molecular cores that commence their phase of collapse from temperatures lesser than 10 K. However, cores with initial temperatures more than 10 K potentially develop, instead of spiral, a ring structure which afterwards experiences the clumps formation. It is possible to observe a transition from spiral to ring instability at a typical initial core temperature of 10 K. Similarly, while investigating the effects of critical density variations on the evolution of protostellar systems, we find that the critical density affects the structural evolution of the envelope of gas, also the dimension of emerging rotating disk structures during collapse too get affected as well as the number of fragments appearing from the concluding fragmentation of the disks. It is suggested that this mechanism has the potential to give birth to young protostellar objects that may eventually constitute systems of bound multiple protostars. The entire numerical experiment is conducted by using 250025 SPH particles to construct virtually the geometry of each molecular core investigated here.
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