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Blood moon why does the moon turn red. ?

WHY DOES THE MOON TURN RED DURING THE LUNAR ECLIPSE?

betelgeuse whats happening there was no clouds?

100 年以后，地球上还有人类吗？？

Initiative of T Crb Global Monitoring Network（Xingming Observatory）

Article from:Xingming ObservatoryInitiator:Xing Gao（高兴） About the Initiative To amateur astronomers with fixed observation sites, I now invite you to join the global monitoring network for the recurrent nova T Coronae Borealis (T CrB) hosted by Xingming Observatory (MPC Code: C42, N86, N88, N89). To join the monitoring network, one should have access to a fixed observation site and fixed observation equipment capable of continuously observing the target, T CrB. At least 20 images need to be taken per observation night, with the ideal scenario being all-night monitoring over an extended period. Large-aperture telescopes are not a must, and even camera lenses are acceptable (though all-sky cams are not recommended due to their relatively low limiting magnitude). The optimal focal length is 400-1000 mm. We do not recommend using telescopes with very long focal lengths (e.g., SCs and RCs), as the field of view is too small. They may not be suitable for photometry due to insufficient comparison stars. Therefore, telescopes with apertures ranging from 80mm to 200mm, which are commonly used by amateur astronomers, are generally the most appropriate. For more information about T Crb, please refer to the following websites: https://www.aavso.org/recurrent-nova-science-tasks-observers-worldwide http://xjltp.china-vo.org/recurrent_nova-schaefer.html (in Chinese) http://xjltp.china-vo.org/tcrb_kepu.html (in Chinese) Currently, historical observation data on the eruption process of this recurrent nova are very scarce. Based on previous similar models, we can only estimate that the nova will erupt within a year, with the full eruption process lasting several hours and potentially featuring a brief ‘plateau’ period. Consequently, the initial observation of the eruption process is of significant importance. This is why we have established a global monitoring network to invite both amateur and professional astronomers from around the world. We will collaborate with a team from Tsinghua University to compile and publish the observation results. If your data is cited, we will invite you to become a co-author of the resulting paper. As mentioned above, the timely processing of the observation data is critical. We have developed a program that can perform photometry on your observation data locally on your computer in real-time. The processed data are then transferred to the server of Xingming Observatory. Since only data, not images, are transferred, the data size for one night potentially being only tens of kilobytes. To use the program, the observer needs to take a few images first and send them to us. We will create an alignment template file (for the program to perform automatic photometry) for you. Participation in the joint observation network is voluntary, and there is no mandatory requirement for how much time one needs to observe during the night. We encourage as many participants as possible and aim for a broad distribution of observations. Our goal is to produce scientifically valuable work and to connect with more individuals in this field. If you are interested in joining the network, please join the T CrB Global Monitoring WeChat group or email us at gaoxing8888@sina.com. Alternatively, you can add me on WeChat (User ID: firststar1974), and I will invite you to the group. Xing Gao（高兴）Xingming Observatory About the target The target for observation is T CrB, with coordinates RA= 15h59m30s and Dec=+25°55′ 13″. It also has other names in different catalogs, such as SAO 84129, HIP 78322, PPM 104498, GSC 2037:1144, B+26 2765, HD 143454, etc. The apparent magnitude is about 10.3. We recommend a field of view of 1 degree by 1 degree. An FoV smaller than 0.5 degrees by 0.5 degrees may not be suitable for this work. (There are some exceptions — please email us for more details. If the FoV is too large (e.g. using a camera lens with a short focal length), image distortion may occur. Then, we suggest using appropriate partial readout when conducting observations, such as using #subframe 0.5 (for ACP scheduling). If you need guidance on the appropriate size of the partial readout, please email us for further discussion. If image file size is a concern, you may also use BIN 4 mode, as long as the program is able to perform photometry properly. We recommend capturing images at a frequency of approximately 1 frame per minute, and capturing a frame less frequently than every 5 minutes is not advised. Additionally, we suggest taking flat, dark, and bias images daily. Although these fields are not required for this program, they are essential for future scientific data processing and calibration if the eruption is detected. Please ensure that the calibration fields match the captured images, namely BIN mode and temperature. Please retain the captured images for at least ten days. The following figure is a reference image of the target (North is on the right). The red circles C1, C2, C3, D1, and D2 in the picture are the comparison stars used by the program to perform differential photometry. Please make sure that these stars are present in the images you are taking. The following figure shows the position and brightness information of each star. It is acceptable as long as the image you capture includes these stars. North does not need to be oriented to the right, and a mirrored image is also acceptable (e.g., if the camera is mounted at the primary focal point). Why to monitor it? Human understanding of recurrent novae is still quite limited. Monitoring T CrB represents an exceptional opportunity for amateur astronomers to contribute to a significant scientific endeavor. The details of its eruption can only be captured through very continuous monitoring. Many aspects of this work are unprecedented, making it a historically significant scientific project. Every day, professionals and amateurs worldwide are closely monitoring its activity, as evidenced by the online data from AAVSO. The race to be the first to detect its eruption is highly competitive. Some screenshots about our program The following is a graph published on the web page. Q&A 1. Can I shoot with a 12-bit digital camera? A: Yes, as long as the file is saved in a 16-bit fits format. 2. What filter should I use? A: If it is a color camera, then just shoot directly. It is recommended not to add light pollution filters or other cut-off filters. If it is a monochrome camera, then please add the three-color R, G, and B filters for photography in front. If it is a photometric filter, you can use V, R, I or Sloan’s g’, r’, i’. You can also capture images without a filter. Please inform us what filter you are using anyway. 3. How long should the exposure time be? A: First, locate to the previous atlas in the article and make sure you captured the right star, T CrB. Please make sure that T CrB is not saturated in the image. Ideally, the ADU (Analog-to-Digital Unit) value of T CrB should be around 10,000. It is necessary to reserve a certain amount of brightness increase space for it, since it is going to erupt. The figure below shows that the maximum ADU value of T CrB is 7,152, with an acceptable signal-to-noise ratio of around 100. 4. How many photos should be taken continuously? A: The more the better, preferably all night, but not less than 20 photos per night. 5. Is the focus required to be very accurate? A: No, overly sharp stars are not conducive for the program to perform photometry. In some cases, appropriate de-focusing is even required, especially when using BIN4 mode. However, avoid defocusing to the point where the stars appear as circles. In principle, it is acceptable as long as the program can recognize the stars. 6. How many sites have already joined the network? A: We will assign a unique number to each site (or individual) that successfully participates in the monitoring. Subsequently, the data collected will be published on our website. The current list of assigned numbers is as follows: TW001 = Vancouver, Canada TW002 = New Mexico, USA TW003 = Chile TW004 = Surrey ,Canada TW005 = California ,USA TE001 = Urumqi Xingming Observatory, China TE002 = Yanqing, Beijing, China TE003 = Wuding, Yunnan, China TE004 = Yinchuan, Ningxia, China TE005 = Pingliang, Gansu, China TE006 = Zhangjiakou, Herbei, China TE007 = Shijiazhuang, Herbei, China TE008 = Qingyuan, Guangdong, China TE009 = Xuyi, Jiangsu, China TE010 = Strand, Norway TE011 = Haba Lake，Ningxia, China 7. Can there be multiple equipment observing at the same site? A: Indeed, the more data we have, the better. There is no conflict, and the data from multiple equipment can support each other. We welcome more observatories and individuals to join us, as this will strengthen our efforts significantly. Disclaimer Participation in this joint observation network is voluntary and conducted cooperatively. If you want to protect your own data and keep them proprietary, please withdraw voluntarily. We do not assume responsibility for disputes caused by the use of related data. While we will make every effort to maximize the value of your data, we cannot guarantee that your data will be used over others’. We will list the relevant participants or team members in the publication. (In principle, a team should not exceed three people). The site can be a commercial remote observatory, but the name of the company or other non-astronomy-related organizations will not be mentioned. If a paper is ultimately published, the selection of co-authors will be decided by the paper’s first author. Neither I, Gao Xing, nor Xingming Observatory will participate in this decision, though we will recommend including individuals who have significantly contributed to the project. Based on past experiences, if the author is not affiliated with a professional astronomical team, the first author generally recommends that the author be affiliated with Xingming Observatory, but this will be at the discretion of the first author. If the author of the paper wishes to use your observation data, please cooperate in protecting the relevant data during the exclusive period to avoid negatively impacting the publication of the paper. For any related issues not mentioned above, I, on behalf of the Xingming Observatory team, reserve the final right of interpretation and will actively coordinate. I hope to avoid any disharmony and thank you for your understanding and cooperation.

T Crb全球监测网络倡议（星明天文台）

文章来自：星明天文台发起人：高兴关于倡议：各位拥有固定观测设备的同好，我现在邀请大家加入到由星明天文台主持的对再发新星北冕座T（T CrB）的全球监测网络。对于加入的要求比较简单，就是要求拍摄地点和拍摄设备相对固定，能够做到对该目标的持续观测即可（每个观测夜至少保证20张以上的图像，最好能长期整夜监测）。对于监测设备的要求也比较低，口径没有限制，甚至相机镜头也可以（但不建议用全天监控，因为极限星等比较有限，竞争力不够），而且不需要大口径，焦距在400-1000毫米最佳，拍摄视场太小可能不适合测量所以并不建议使用焦距过长的望远镜，爱好者常用的口径80mm到200mm之间的望远镜效果最好。有关该再发新星的资料可以阅读： http://xjltp.china-vo.org/recurrent_nova-schaefer.html http://xjltp.china-vo.org/tcrb_kepu.html 目前对于该再发新星的爆发过程的历史观测资料很稀少，只能从一些先前的类似模型大致估计即将在未来1年内爆发，而且爆发过程可能预计在几个小时内，且在爆发过程中可能出现短暂平台期，因此对于该变星爆发第一缕光的观测意义非常重大，这也就是我们组织全球监测网络的原因所在，我们诚挚邀请全球各地同好加入进来（欢迎外国盆友），我们也联系了清华大学的专业天文团队对观测成果进行总结发表，如果您的数据得到引用，我们也邀请您成为论文的合作作者之一。如上所述，对于该目标的观测数据的及时处理是关键，我们开发了一个应用程序，可以实时对您的观测数据在观测计算机本地进行测量并将测光数据结果实时传输到星明天文台的服务器上（因为不传输图像只传数据，所以基本不占用带宽，一晚上的数据量可能只有几十K），为了保护观测人的数据，我们在网络上大约晚10分钟发布（基本算是实时发布了），我相信这个爆发的第一发现的竞争已经激烈到半小时内。对于应用程序的准备，需要观测者先拍摄几张原始图像发给我，我需要做一个程序测量定标模版，并按照程序说明要求建立文件名和目录名的规则即可。加入该联测团队是自愿行为，也对加入人员无观测时间的固定要求，我们期望加入者越多越好，分布范围越广越好，以期做出更有科学价值的工作，也期望以星会友。如果有意向加入，请加T CrB全球监测微信群，或者给我发邮件gaoxing8888@sina.com 星明天文台：高兴关于拍摄目标：我们拍摄的目标名称叫 T CrB，坐标是赤经：15 59 30 赤纬：+25 55 13，在不同的星图中它还有其他别名，比如SAO 84129，HIP 78322，PPM 104498，GSC 2037:1144，B+26 2765，HD 143454等等，视亮度大概是10.3等。我们推荐的图像拍摄视场是1度*1度为佳，如果视场小于半度*半度，可能不适合做此工作，当然也可以特殊处理，可以联系我，如果视场太大（比如你使用焦距比较短的相机镜头），考虑到大视场像场畸变，可能不利于观测图像与模版图像对齐，那么我建议你拍摄的时候使用适当的局部读出，比如使用#subframe 0.5这样的设置（对于ACP排程观测计划来说），至于什么是合适尺寸的局部读出，这个可以找我联系，发给我原图，然后再沟通。如果你觉得拍摄图像的文件占用空间太大，也可以用BIN 4来进行拍摄，只要程序测试过关就没问题。我们建议拍摄的频率在1分钟1张就可以，多张也没问题，但不建议超过每5分钟拍摄一张。对于拍摄的原始文件，建议至少保留10天以上的数据，以备未来有价值时进行精确测量，我们建议每天拍摄平场暗场和偏置场，虽然本程序不需要这些场，但如果是你发现了爆发，那么日后的科学数据处理需要这些场做校准才更有科学性（校准场格式需要和拍摄的图像一致，比如像素数和温度等）。下图是北在右边的拍摄图像的参考图图中红圈的C1,C2,C3,D1,D2是程序比较测光用到的星点，请保证拍摄图像中有这些星就可以。下图是THE SKY软件模拟的各星点的位置和亮度信息你拍摄的图像中能包含这些星点就OK，不需要北在右边，镜像也可以（如果是主焦点望远镜会镜像），也不用担心德式赤道仪翻身导致图像旋转180问题，如果是地平式跟踪，图像有场旋也不影响监测。关于我们监测的目的：人类对再发新星知之甚少，可以说T CrB是目前爱好者能参与的最佳目标，对于它爆发的过程，只有通过这次爆发的极早期监测得到，很多工作是史无前例的，是具有一定历史意义的重要科学工作，全球每天有无数专业和业余爱好者在时刻监视着它的一举一动，这一点从AAVSO的在线数据就可以看到，谁能是第一个发现其爆发的人，可谓竞争相当激烈。根据以往一些论文模型我们预计这次爆发会增亮到2等亮度，增亮幅度达到8等，而且增亮过程时间可能在10小时的数量级，而且增亮过程还有可能出现波动平台期等细节情况，有可能先增亮2个星等到8等左右，停留一定时间再次增亮，这些都不得而知，因此发现它爆发的第一缕光成了很有意义的事情，从细节来说，也许不同波段（颜色）的增亮是不同步的，对它的多色观测也意义非凡，因此，比如用全天摄像头进行监测是不能够及时发现的（因为全天相机的极限星等不够，一般只能达到8等左右），用每隔几个小时拍摄一张的模式也是会丢失机会的，再加上全球都盯着（因为有预报，就像流星雨预报那样，虽不准确，但不可不信），竞争可以用惨烈来形容，这就需要大家联合起来共同监测才能占得先机，而且对数据的实时处理和响应成为关键。我们根据现有情况自己编写了相关的在线实时处理发布程序，这让这个合作成为可能，而且我们希望有更多的站点加入进来，毕竟不可能观测点都是晴天。关于数据处理程序：这是一个用来监测T CrB爆发的通用程序，其功能就是利用各个远程台自愿提供的观测数据，在远程计算机进行初步处理并将数据传送到服务器并发布，同时进行监测预警。考虑到通用性以及实时数据所有权，光变曲线数据展示以png图像展示在固定网页端并延时10分钟发布。使用本程序前，需要用户提供至少两张拍摄的包含T CrB的图像作为模版（如果使用滤镜，则需要各色滤镜提供两张），要求用户保持拍摄模式和模版一致，比如总像素数量和BIN值要与模板一样，相机制冷温度一致，曝光不要差距过大并最好固定不变，如果有可能最好保持图像的方位角（相机的方位角）固定（比如正北方向）焦点不需要很准确，需要提供的两张模版图像，一张信噪比较好一张信噪比较差，可以考虑用拍摄时接近中天的一张图，和接近低地平的一张图由于是简单比较测光，所以不要求提供暗场偏置和平场，如果能在亮场图像输出的时候软件自动校准了那更好。用户需要将模版文件传给我，我需要做星点定位，然后命名为类似template1.fits（或者类似B_template1.fits，G_template1.fits）和template2.fits，回传给用户，请将两文件放在本程序指定的主目录下的template目录下本程序使用tcp-ip方式传输T CrB及周围5颗比较星的测光数据，不传输和回传其他任何数据，无任何其他与本程序观测目标无关的越权非安全代码，也请大家帮助保护服务器安全，不要私下转传本程序。以下是程序的一些说明： # 请将RUN.bat，cfg.txt和T_CrB_2024xxxx-client.exe三个文件放在某个目录下，并编辑RUN.bat文件（右键该文件点编辑）， # 将set My_PATH=部分填写成程序所有目录，如：set My_PATH=D:\T_CrB，将最后一行的–dir之后改为需要处理的监测图像文件的上一级目录，例如–dir D:\ T_CrB_monitor # –dir之后的内容是告诉程序需要监测的“主目录”，比如常见的是D:\T_CrB_monitor，程序要求拍摄的T CrB的文件必须存放在这个监测目录下的某年某月某日的目录下，比如D:\T_CrB_monitor\20240628或者D:\T_CrB_monitor\2024-06-28 # 本程序用来进行T CrB的监测，一般运行RUN.BAT文件就可以，并且运行后只要不关闭cmd显示窗口，程序就会自动完成观测数据的处理和数据上传 # 存放的文件名称满足格式：T_CrB*.f*，也就是说必须以T_CrB开头（注意下划线），后缀名必须以f开头，比如：T_CrB_UTC20240613_054759-B-020S_E_-10C.fts # 程序运行前，要求在“主目录（也就是–dir指示的目录）”下建立一个template目录，并将确定的两个（或者多个）模版文件存放在该目录下，一般命名为template1.fits和template2.fits，一般template1.fits的是信噪比比较好的，template2.fits是信噪比比较差的图像模板 # 程序运行时，会每大约半分钟进行一次处理，刚运行时可能需要等待一下，程序打包比较大，用python语言写成。关闭cmd窗口即退出运行，程序不需要每天都开启，只要不关闭，就是在实时监视目录中的最新目录下的新文件进行处理（程序每次运行只会处理最新目录的数据，之前日期的数据不会处理），如果发现程序停在某个时间不动，那么可能需要关闭并重新开启，程序运行会产生一个处理目录下的所有文件集合组成的txt文本，可以打开查看，过期的可以删除。以下是程序常见位置截图以及程序运行情况截图以下是网页发布测量展示图片 Q&A: 1.12位的数码相机拍摄是否可以？ A:可以，只要文件保存成fits16位格式就可以 2.用什么滤镜拍摄？ A:如果是彩色相机，那么就直接拍摄就行，建议不要加光害或者其他截止滤镜，更不需要用窄带。如果是单色相机，那么前面加摄影用R,G,B滤镜三色就可，如果是测光滤镜，可以用V,R,I或者用斯隆的g’,r’,I’就可以。单色相机无滤镜也可以，但都需要告知我。 3.曝光多久？ A:首先找到前面文章中的贴图，对应好目标星，主要T CrB不饱和就可以，但最好让T CrB的ADU值在10000左右就可以，毕竟以后它要爆发，还需要给它预留一定的亮度上升空间，甚至可以进一步减小。下图展示了T CrB的ADU最大值是7152，信噪比在100左右已经很好。 4.连续拍摄多少张？ A:越多越好，最好整晚，但不得少于20张。 5.焦点要求很准确吗？ A:不要求，太细的星点反而不利于程序识别，甚至某些设备考虑到BIN4拍摄，可能还需要适当的散焦，但不要散焦太厉害到一个圈就OK，原则上就是程序能识别就好。 6.我们已经有多少站点进行联测了？ A:我会给能够成功监测的站点（个人）一个编号，然后以后数据会发布在网页上，目前的编号有 TW001=加拿大温哥华TW002=美国新墨西哥州TW003=智利TW004=加拿大素里TW005=美国加州TW006=美国内华达州TE001=乌鲁木齐星明天文台TE002=北京延庆TE003=云南武定TE004=宁夏银川TE005=甘肃平凉TE006=河北张家口TE007=河北石家庄TE008=广东清远TE009=南京盱眙TE010=挪威StrandTE011=宁夏哈巴湖 7.同一个站点可以多个观测者吗？ A：可以，多多益善，不冲突，相互数据还可以佐证，我们非常欢迎更多的站点加入，会更有力量。声明：本次联测的加入属于自愿原则，合作开展，如果对自我数据要求保护，不满足我们前面提到的数据发布要求的请自觉退出。我们不承担对相关数据使用问题带来的纠纷责任。我们会尽量让各位的数据使用价值最大化，但不承诺会使用谁的数据而不采用谁的，如果上报，我们会在报告中罗列相关参与人员或者团队成员（请提前说明，原则一个团队成员不超过三人），联测站点可以是商业远程天文台，但不标注公司等非天文观测台址名称。如果最终发表论文，论文合作作者的署名由论文第一作者决定，我本人及星明台不参与其中的决定，但会对本联测项目起到一定作用的人员进行署名推荐，根据以往经验，如果署名作者非天文专业单位，论文一作一般会建议署名作者挂靠星明天文台为作者单位，这些由论文一作决定。如果论文作者欲使用您的观测数据，请配合做好相关数据独占期内的保护工作，以免对其论文发表带来负面影响。对上文未提及的相关问题，我代表星明天文台团队具有最终解释权，也会积极协调，不情愿看到不和谐的事情发生，多谢大家理解和配合。

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