本文關(guān)鍵詞：射電望遠(yuǎn)鏡無(wú)線電干擾監(jiān)測(cè)方法和數(shù)據(jù)分析的研究　出處：《西安電子科技大學(xué)》2015年碩士論文　論文類型：學(xué)位論文

  更多相關(guān)文章： 射電望遠(yuǎn)鏡 無(wú)線電干擾 頻譜監(jiān)測(cè) 測(cè)試系統(tǒng) 選址

【摘要】：射電天文使用高靈敏度的設(shè)備測(cè)量來(lái)自宇宙由于自然現(xiàn)象發(fā)射的特定頻率的信號(hào),以此來(lái)研究自然現(xiàn)象。其站址的選擇是射電望遠(yuǎn)鏡完成既定科學(xué)目標(biāo)并有效運(yùn)行的首要條件,選址的主要因素有電磁環(huán)境、水文、氣象、地質(zhì)、可及性和當(dāng)?shù)乇Ｕ蠗l件等。射電天文的發(fā)展追求高靈敏度的數(shù)據(jù),這要求在更寬頻率上觀測(cè),隨著觀測(cè)方法和技術(shù)的發(fā)展,原來(lái)分配的頻段已不夠使用。隨著各類無(wú)線電主動(dòng)業(yè)務(wù)的不斷發(fā)展,人類使用無(wú)線電通訊占用越來(lái)越多的頻段,使用地域亦不斷擴(kuò)大。射電望遠(yuǎn)鏡需要躲避無(wú)線電干擾(RFI),選擇電磁環(huán)境優(yōu)良的站址,保護(hù)電磁環(huán)境。同時(shí)RFI的監(jiān)測(cè)結(jié)果也為接收機(jī)系統(tǒng)的研制,站址內(nèi)無(wú)線電干擾查找和射電寧?kù)o區(qū)的建立和保護(hù)提供依據(jù)。首先列出了國(guó)際上和我國(guó)射電天文業(yè)務(wù)的工作頻率和科學(xué)日標(biāo),給出了國(guó)內(nèi)射電望遠(yuǎn)鏡的實(shí)際使用頻段。結(jié)合國(guó)際電聯(lián)對(duì)射電望遠(yuǎn)鏡的無(wú)線電干擾的標(biāo)準(zhǔn),給出了國(guó)內(nèi)典型射電望遠(yuǎn)鏡的干擾門(mén)限和干擾時(shí)間要求。然后研究了國(guó)際上針對(duì)SKA(Square Kilometer Array)選址在2003年和2010年進(jìn)行的兩輪測(cè)試的測(cè)試方法和RFI監(jiān)測(cè)設(shè)備,結(jié)合射電望遠(yuǎn)鏡選址和RFI監(jiān)測(cè)的實(shí)際工作,提出合適的無(wú)線電干擾測(cè)試方法,討論如何建立射電望遠(yuǎn)鏡電磁環(huán)境選址測(cè)試裝置(包括軟、硬件、數(shù)據(jù)處理等)。最后對(duì)目前我國(guó)在建和預(yù)研階段的部分射電望遠(yuǎn)鏡臺(tái)址進(jìn)行現(xiàn)場(chǎng)測(cè)試,對(duì)于數(shù)據(jù)的處理方式主要采用統(tǒng)計(jì)的方法,根據(jù)監(jiān)測(cè)得到的站址RFI數(shù)據(jù),分析站址的RFI的特性和業(yè)務(wù)分布,在電磁環(huán)境層面上分析站址的優(yōu)劣。由于望遠(yuǎn)鏡具有極大的接收面積和良好的接收機(jī)系統(tǒng),國(guó)際電聯(lián)給出的干擾標(biāo)準(zhǔn)要求很高。目前的RFI監(jiān)測(cè)設(shè)備靈敏度達(dá)不到電聯(lián)規(guī)定要求的射電望遠(yuǎn)鏡干擾門(mén)限,需要研制靈敏度更高的RFI監(jiān)測(cè)設(shè)備不斷接近或達(dá)到該門(mén)限。同時(shí)在以后的選址工作中,積累測(cè)試數(shù)據(jù),對(duì)數(shù)據(jù)進(jìn)行分析和比較,了解無(wú)線電業(yè)務(wù)的發(fā)展和變化,作為以后進(jìn)行射電天文觀測(cè)和保護(hù)電磁環(huán)境的依據(jù)。
[Abstract]:Radio astronomy uses highly sensitive equipment to measure signals from specific frequencies emitted by natural phenomena in the universe. The site selection is the primary condition for the radio telescope to complete the established scientific objectives and operate effectively. The main factors of site selection are electromagnetic environment, hydrology, meteorology and geology. The development of radio astronomy pursues highly sensitive data, which requires observation at a wider frequency, with the development of observational methods and techniques. With the continuous development of all kinds of active radio services, the human use of radio communication occupies more and more frequency bands. The radio telescope needs to avoid radio interference, select the site with good electromagnetic environment and protect the electromagnetic environment. At the same time, the monitoring results of RFI are also for the development of receiver system. The radio interference search and the establishment and protection of radio quiet area within the station site are provided. Firstly, the working frequency and scientific day standard of radio astronomical service are listed both internationally and in China. The practical frequency band of domestic radio telescope and the radio interference standard of ITU to radio telescope are given. The interference threshold and interference time requirements of typical domestic radio telescopes are given, and then the international targets for SKA(Square Kilometer are studied. Two rounds of testing methods and RFI monitoring equipment were selected on 2003 and 2010. Combined with the actual work of radio telescope site selection and RFI monitoring, this paper puts forward a suitable radio interference testing method, and discusses how to establish a radio telescope electromagnetic environment location testing device (including software and hardware). Finally, the site of some radio telescopes in the stage of construction and pre-research in our country is tested on the spot, and the statistical method is mainly used to deal with the data. According to the monitoring site RFI data, the characteristics and service distribution of site RFI are analyzed. The merits and demerits of the station are analyzed on the level of electromagnetic environment. The telescope has a large receiving area and a good receiver system. The interference standard of ITU is very high. The sensitivity of the current RFI monitoring equipment is not up to the interference threshold required by ITU for radio telescopes. It is necessary to develop more sensitive RFI monitoring equipment to approach or reach the threshold. At the same time, in the later site selection work, the test data should be accumulated, and the data will be analyzed and compared. To understand the development and changes of radio service as a basis for future radio astronomical observation and protection of electromagnetic environment.
【學(xué)位授予單位】：西安電子科技大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2015
【分類號(hào)】：P111.44

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相關(guān)期刊論文 前2條

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本文編號(hào)：1369519